Open Collections

UBC Theses and Dissertations

UBC Theses Logo

UBC Theses and Dissertations

Inversion of cosmogenic nuclide data from iron meteorites Pearce, Steven James 1984

Your browser doesn't seem to have a PDF viewer, please download the PDF to view this item.

Item Metadata

Download

Media
831-UBC_1984_A6_7 P42_7.pdf [ 4.7MB ]
Metadata
JSON: 831-1.0085783.json
JSON-LD: 831-1.0085783-ld.json
RDF/XML (Pretty): 831-1.0085783-rdf.xml
RDF/JSON: 831-1.0085783-rdf.json
Turtle: 831-1.0085783-turtle.txt
N-Triples: 831-1.0085783-rdf-ntriples.txt
Original Record: 831-1.0085783-source.json
Full Text
831-1.0085783-fulltext.txt
Citation
831-1.0085783.ris

Full Text

INVERSION OF COSMOGENIC NUCLIDE DATA FROM IRON METEORITES  by-  Steven James Pearce  B.Sc.  (Hon), University of British Columbia, 1981  A THESIS SUBMITTED  IN PARTIAL  T H E REQUIREMENTS MASTER  FULFILMENT OF  FOR T H E DEGREE O F O F SCIENCE  in THE FACULTY OF GRADUATE  STUDIES  (Department of' Geophysics and Astronomy)  We  accept this thesis as conforming to the required standard  T H E UNIVERSITY  O F BRITISH  COLUMBIA  August, 1984  Steven James Pearce, 1984  In p r e s e n t i n g  t h i s t h e s i s i n p a r t i a l f u l f i l m e n t of  requirements f o r an advanced degree a t the  the  University  o f B r i t i s h Columbia, I agree t h a t the L i b r a r y s h a l l make it  f r e e l y a v a i l a b l e f o r reference  and  study.  I  further  agree t h a t p e r m i s s i o n f o r e x t e n s i v e copying o f t h i s t h e s i s f o r s c h o l a r l y purposes may  be  department o r by h i s or her  granted by  the head o f  representatives.  my  It i s  understood t h a t copying or p u b l i c a t i o n o f t h i s t h e s i s f o r f i n a n c i a l gain  s h a l l not be  allowed w i t h o u t my  permission.  Department o f  /O  The U n i v e r s i t y o f B r i t i s h 1956 Main Mall Vancouver, Canada V6T 1Y3 r  Date  DE-6  (3/81)  9/ Alit  .  *j Asmo Kid7 * y Columbia  written  ABSTRACT The long accepted conclusion that the galactic cosmic ray flux has been "fairly" constant  over the  self-inconsistent diserepency  past  billion years. or so  is  based  upon both  weak  inferences  and  interpretations of the data. For example, the well known exposure age  between  the  analyses  based  on  4 0  K  and  those  of  the  shorter-lived  radionuclides (i.e., Be, " A l , and C1) has yet to be properly reconciled. Recent work 36  10  by  Schaeffer  et  al.  (1981)  on  space  erosion  rates  for  irons  suggests  that  only  a  variation in the galactic cosmic ray flux yields the satisfactory explanation. Reformulating  this  problem  (Backus and Gilbert, 1967, 1968,  within  the  framework  of  linear  inverse  theory  1970) allows for an unprecedented perspective on this  problem as compared with any previous analyses. In theory, it is found that smoothed estimates of the long term galactic cosmic ray prehistory can be formed with arbitrarily good resolution. The degree of smoothing is  determined  meteorite  primarily  samples  by  the  relative  exposure  as well as their associated  age  experimental  differences  among  uncertainties.  adjacent  Moreover, this  is the only unique information available to this entire study. The near absense of a priori constraints promotes a simple objective philosophy of  interpretation.  Further,  the  lack  of  any  independent  exposure  age  determination  presents an inherent non-linearity. But, it can be shown that a single model for both the  cosmic  ray flux  and the  exposure  ages, mutually consistent  with the  and associated errors, can be derived under several fundamental criteria.  observations  i i i  TABLE OF CONTENTS  ABSTRACT  ii  TABLE OF CONTENTS  iii  LIST OF TABLES  iv  LIST OF FIGURES  v  ACKNOWLEDGEMENTS  vii  1  INTRODUCTION  1  2  ESSENTIALS OF THE COSMOGENIC NUCLIDE PROBLEM  6  3  4  5  2.1 2.2  Cosmic Radiation Pertinent Nuclear Chemistry  2.3  Meteoritic Data and the Fatal Gap  .'.  7 13 23  ANALYTIC STATEMENTS OF THE FORWARD PROBLEM  33  3.1 3.2 3.3  Thin Target Production Rates Thick Target Considerations Problems and Assumptions  34 36 45  3.4  Functional Description of Cosmogenic Nuclide Abundances  52  RESOLUTION ON THE GALACTIC COSMIC RAY PREHISTORY  56  4.1 Derivation of the Resolving Kernels 4.2 . Single Sample Analysis  57 61  4.3  66  Multi- Sample Analysis  MODELLING THE LONG TERM IRRADIATION PREHISTORY 5.1 5.2 5.3 5.4  Derivation of the Flattest Model Data and Estimates of Uncertainties Contending with Non-Linearity Results and Conclusions  71 71 76 81 86  REFERENCES  92  APPENDIX A  97  APPENDIX B  99  APPENDIX C  101  iv  LIST OF TABLES  Table 2.1:  Composition of Galactic Radiation  8  Table 3.1:  Effective Irradiation Hardness Indicators  40  Table 3.2:  The Depth Dependent Energy Spectrum  43  Table 5.1:  Data for Use in the Long Term Irradiation Problem  78  V LIST OF FIGURES  Figure 1.1:  The Ideal Description of the Cosmogenic Nuclide Problem  Figure 2.1:  Cosmic Ray Classification and Nomenclature  11  Figure 2.2:  Mass Yield Curves  16  Figure 2.3:  Excitation Functions for Low Energy Reactions  19  Figure 2.4:  Excitation Functions for High Energy Reactions  19  Figure 2.5:  Exposure Age Histograms  24  Figure 2.6:  Excitation Functions for K Production in a Typical Iron  Figure 2.7:  Cosmic Ray Produced Radionulides Found in Iron Meteorites  29  Figure 2.8:  Orbits of Three Chondrites  31  Figure 2.9:  The Radial Modulation of Galactic Cosmic Radiation in the Solar System ... 31  Figure 3.1:  ,  40  2  27  He Contours in a Meteorite Cross Section  37  Figure 3.2:  Calculated Specific Production Rates of Be. "Al, and "CI  39  Figure 3.3:  Radial Variation of Some Inert Isotopes in Iron  40  Figure 3.4:  The Differential Energy Spectrum at 100 g-cnr  1  42  Figure 3.5:  Depth Dependent Parameters for Energy Spectra  44  Figure 3.6:  The Energy Dependence of Cosmogenic Nuclide Production  48  3  10  vi  Figure  4.1:  Averaging Functions for Four Different Decades of Exposure Age  62  Figure  4.2:  Averaging Surfaces for Exposure Ages of IO and 10 Years  63  Figure  4.3:  Averaging Surface for an Exposure Age of 10 Years  65  Figure  4.4:  Averaging Surface for the Two-Sample Problem  67  Figure  4.5:  Schematic of Designing Optimal Resolution  68  Figure  4.6:  Averaging Surface for the Two-Sample Problem (High Resolution)  69  Figure  5.1:  Flattest Models Based Upon Synthetic Data and Varying Age  82  Figure  5.2:  Flattest Models Based Upon Synthetic Data and Varying Age  83  Figure  5.3:  Contour Plot of Lj-Norm in the 2-Sample Problem  85  Figure  5.4:  Model Norms Based Upon the ML Ayliff Iron Meteorite  87  Figure  5.5:  Flattest Models Based Upon the M L Ayliff Iron Meteorite  88  Figure  5.6:  Global Flattest Models for Four Different Iron Meteorites  89  6  7  7  Vll  ACKNOWLEDGEMENTS  Having spent the better part of two consequtive years on a problem that is scarcely older than four decades conjures a sensation of belonging. Part of this response is clearly due to my association with many interested individuals whom I have had the pleasure of introducing this topic. In my case however, the individual who got the proverbial wheel rolling is my supervisor Prof. R. Don Russell. I am honoured to have been his student, and in retrospect I am grateful for the quality of his teachings. I thank him dearly for this second and ever more fascinating guided tour of research. On  the other hand, I would also like to take this opportunity  to express deepest  thanks to Prof. Masatake Honda on behalf of both Prof. Russell and myself for providing the initial impetus. I owe special thanks to Prof. D. W. Oldenburg for introducing me to inverse theory in his typically lucid manner. Moreover, his criticisms have been indispensible. His enthusiasm about this problem cannot be overstated. In addition, special thanks is due to Dr. B. Narod for his numerous contributions of both his time and of his many technical talents that greatly facilitated the development of this thesis. Furthermore, a great deal of my time and effort was  spared by Mr. Kerry Stinson who played an essential role in my education on the  application of inverse theory to this problem. I'm sure that he found his involvement with this topic to be most rewarding. Many thanks Kerry! This department has been particularly suitable for the pursuit of this problem as it is a topic in geophysical data analysis applied to high energy astrophysics. Of the astronomy group, Prof. G. A. H. Walker has been "instrumental" in exposing certain key information to me which otherwise would have gone unnoticed.  VI  One  of the principal highlights of my  11  past two years as a graduate student was  meeting Prof. Peter Jeffery. Moreover, I had the privilege of involving him in this topic. However, his advice went far beyond just that of academia. I am deeply indebted to him. My  initial understanding of this thesis was  greatly facilitated by members of the  Department of Chemistry at Simon Fraser University. In particular, 1 wish to express sincere thanks to Prof. R. Korteling for the many hours of personal education he provided me with. Special thanks go as well to Prof. J. D'Auria and Prof. D. Boal of the same department. In addition, I have had the privilege of sharing adjacent offices with Mr. Toshifumi Matsuoka. Our common interests have somewhat tied us into each others respective research interests. More important however I have found an important friend. I must also acknowledge Mr. Mark Lane, Mr. Robert  Glenn Scharein, and  Mr. Thomas Goulet for their useful  conversations concerning this problem. Again however, it is their friendship that I am most grateful for. Finally, I thank my family for their patience and understanding throughout this period. Their love and support made it all run so smoothly!  1 1  INTRODUCTION  Over four decades ago a geochronological study of several iron meteorites employing the He-U method produced a perplexing scatter of ages (Arrol et al^ 1942), several greatly exceeding the current canonical age of the solar system. In an attempt to reconcile with the oldest ages Bauer (1947) and Huntley (1948) independently suggested that He is efficiently 4  produced by cosmic ray interactions with meteorites while in interplanetary space. If this were so then He was. also expected to be anomalously 3  abundant in the samples. Subsequent  analysis revealed the ratio He/ He to be of order unity in meteorites (Paneth et al., 1952) 3  4  in contrast to the primordial helium ratio of roughly IO (Tolstikhin, 1978). Similar anomalies 1  4  were observed for the isotopes of neon (Reasbeck and Mayne, 1955) and argon (Gentner and Zahringer, 1957). Moreover, short- lived radioisotopes are observed in freshly fallen meteorites, lunar samples, and retrieved spacecraft All such observations give overwhelming support to the Bauer-Huntley hypothesis which has long since been accepted as fact Isotopes produced in matter interacting with cosmic radiation are generically known as cosmogenic nuclides. A simple description concerning the physics of this problem is identical to that of a particle beam accelerator experiment in which a target of known composition is exposed to a high energy incident particle flux for an arbitrary time T. Some high energy nuclear (spallation) reactions will occur between incident species and target isotopes resulting in the accumulation of product nuclides (interaction debris) within the body. The nature of the spallation process allows for the production of any isotope of atomic mass below that of the target nuclides. A key goal for accelerator experiments is the empirical determination of product yields, information crucial to the interpretation of cosmogenic nuclide data. Unlike a  'This refers to the helium abundances trapped during the condensation of the solar nebula. It is the largest helium ratio observed in the solar system apart from cosmic ray interaction products and cosmic rays themselves.  2 controlled laboratory experiment however the history of both target and irradiation conditions are unknown in the cosmogenic nuclide problem. It is assumed that there exists some collisional  and/or  erosional process  responsible  for producing  interplanetary debris with  dimensions corresponding to the mean free path of cosmic ray particles within the body. The 1  ideal description involves an initially shielded fragment suddenly exposed to the cosmic radiation. Certain  "cosmogenic  clocks" of interest are subsequently switched  on and the  meteoroid continues uneventfully in its orbiL After a clearly defined exposure time the body encounters the earth and becomes reshielded by the atmosphere.  age. Space erosion will be discussed in section (2.3).  'A few meters in stone or iron.  3  The  traditional objectives of cosmogenic nuclide research have been twofold. One  approach addresses the galactic cosmic ray flux prehistory and is consequently interest to high  energy astrophysicists. The other viewpoint  of greatest  concerns the chronology of  meteoroids as small bodies in the solar system and hence is of principal interest to researchers of meteoritics and the planetary sciences. In simple terms, the mutual goals are to derive information on both the unknown time dependence of a particle flux and the unknown  exposure time of a target using measured abundances of spallation products in tandem with experimentally determined yields. Clearly, the two desired quantities depend upon one another . __. in^ the interpretation of „the_ data. Moreover, independent a priori knowledge which can be used to constrain either the flux or meteoroid prehistory is grossly inadequate. Consequently, the natural dichotomy of the problem arises when researchers primarily interested in exposure ages are forced to make strict assumptions on the flux prehistory and vice versa. Evidently, the current status of this problem allows for many traps. Although  research has  been  rewarding where valid inferences can be drawn, unfortunately, questionable practices exist in the literature. It is currently held that the galactic cosmic ray flux has been constant to within experimental precision. In fact, these conclusions were originally based upon the analysis of radionuclides with half-lives on the order of 10 years and less (Arnold et al., 1961). The 6  validity of the constant flux model over this time frame is easily demonstrated (see Appendix A). However, there is strong evidence to suggest that this model is incorrect over greater time scales. The analysis of K, the next radionuclide with respect to increasing half-life that 40  is produced in appreciable yield within meteorites, indicates that there has been a general increase of the galactic flux over the past 10' years. The only competing interpretation of the 40  K observations, space erosion, is apparently inadequate (Schaeffer et al., 1981). Nevertheless,  the constant flux model is widely assumed over a gigayear throughout the literature resulting in self-inconsistent interpretations of the data.  4 Another misconception  in this problem is the tendency to assume that continually  improved observations inevitably lead to increasingly accurate understandings.  All  physical  problems possess inherent limits to the interpretation of real observables regardless of their quantity and quality. For a given problem one could spend great time and effort to amass an arsenal of data only to find marginal improvements over the explicative powers of a few crude observations. Let us now take a broader perspective on the problem of interpreting abundances of cosmogenic nuclides. Clearly, using these data to say something meaningful about prehistoric irradiation conditions is an exercise in inference based upon indirect observations. Over the past few years this familiar class of problem has undergone a significant advance and the philosophy of such has come to be known as inverse theory There are two general kinds of inverse problems depending upon whether or not the working equations are linear. There is presently little known about the solutions of non-linear inverse problems and so it is usual to elicit assumptions which reduce them to linear ones. If a problem can be posed linearly then inverse theory becomes a robust framework from which to address key questions concerning the innate information capacity of the data, effects of observational uncertainties, experimental design, and the construction of models. The  goal of this paper is to reformulate the cosmogenic nuclide problem through  inverse theory. It is claimed that this analysis affords a substantial advantage over traditional methods. In particular, attention will be focused on the long term problem (~10' years) based upon the analysis of existing data from iron meteorites. An attempt is made to present a broad overview of the possible interpretations and the limitations therein. In addition, it is clearly shown where effective improvements to the problem can be made. Moreover, it is  "Much of the earlier developmental work dealt with problems concerning geo- and planetary physics. Consequently, the field is also known as geophysical inverse theory.  5  demonstrated  how  objective models of the galactic cosmic  ray flux prehistory can be  constructed which are mutually consistent with all current observations. The goal of this paper hereafter is to set upon these problems. It is assumed that the reader has some familiarity with inverse theory. However, this 1  is not essential as the work presented here is largely self-contained. In what follows the description of all physical processes, and assumptions therin, crucial to understanding the origin of observables is henceforth referred to as the forward problem. Conversely, the procedure by which the-data are implemented- for the purpose of_ inferring the prehistory of one or more physical quantities akin to the forward problem is henceforth referred to as the inverse problem. As such, the inverse problem  is intangible until the  forward problem is adequately understood. The intent of the next two chapters is to adequatly review and codify the forward problem so that proper attention can be given to inversion. The reader may. wish to refer to one  or more  reviews  on  the cosmogenic  nuclide problem  for further  details (i.e.,  Schaeffer, 1962; Geiss et al., 1962; Honda and Arnold, 1967; Kohman and Bender, 1967; Kirsten and Schaeffer, 1971; Lai, 1972). Later chapters will be concerned with inversion itself.  An excellent review of inverse theory was given by Parker (1977). In addition, Twomey (1977) provides a comprehensive overview of the subject However, the actual analysis presented in this work is largely based upon the series ofrigorouspapers by Backus and Gilbert (1967, 1968, 1970). J  6  2  ESSENTIALS OF THE COSMOGENIC NUCLIDE PROBLEM  Cosmogenic  nuclide  production may  be viewed  as consisting  of three primary  phenomena, respectively, concerned with the nature of i)  the incident particle flux (i.e., cosmic radiation),  ii)  the. matter interaction mechanisms (i.e., pertinent nuclear chemistry), and  iii)  the target (i.e., meleoroids, cosmic dust, lunar surface, spacecraft, etc.).  The forward problem entails a thorough enough physical understanding of i), ii), and iii), as well as adequate knowledge concerning the histories of i) and iii), to allow for predictions of cosmogenic nuclide abundances. Of course, the inverse problem also invokes physical insight into all three components. However, independent information on the history of either the cosmic ray flux or the target is sparse and highly conjectural. Consequently, it becomes necessary to define a quantity which describes the progression of both the cosmic radiation and the target in time; namely, the irradiation history. Thus, the actual goal of the inverse problem is to use observed cosmogenic nuclide abundances to recover information on the irradiation prehistory,  related to the target(s) under study, based  upon current physical  understandings of i), ii), and iii).  1  The purpose of this chapter is to present the required understanding of these three components for the purpose of describing the forward problem. Effort is made to provide extended references wherever appropriate as only those aspects of immediate concern to this work are addressed.  •We elicit this important concept in order to emphasize that the current status of the cosmogenic nuclide problem does not properly allow one to address either the flux or target prehistory separately over long time scales.  7 2.1  Cosmic Radiation:  The term cosmic ray applies to high energy  1  particles or quanta of extraterrestrial  origin. Although the existence of cosmic radiation has been known for over seventy years fundamental questions concerning their origins and large scale distributions are still inadequately understood. Nearly all that is known about such problems comes from indirect observations of one form or another. Such knowledge is crucial to understanding possible long term variations of the galactic flux which should be observed from the inner solar system. One would "  assume that.-these issues, should be brought forth in order to provide necessary a priori information to assist in restricting the possible interpretations. Indeed, even a cursory overview of the arguments that support the current concensus of interpretations among cosmic ray researchers would be an overwhelming undertaking (i.e., Brecher and Burbidge, 1972; Cesarsky, 1980; Longair, 1981). Moreover, we shall see that the results of inversion presented in this work do not possess adequate detail to warrent the effort Rather, it is natural to view the results contained herein as an additional indirect observation of the galactic cosmic ray flux to further assist in the understanding of the origin and distribution problems. In this work interest lies primarily in quantitatively understanding those aspects of the incident flux that are essential to the development of the forward problem (i.e., composition, flux, energy spectra, arrival directions etc.). Let us begin with a general description of energetic particles observed near the earth. In 1942, it was found that particles with energies in excess of 1 MeV originating at the sun can encounter the earth (Forbush, 1946). The steady emission of lower energy particles, the so-called solar wind, was later confirmed by experimental results from unmanned spacecraft. Unlike  the solar  wind  •Loosely defined to be above 1 MeV.  however  the high  energy  component  is emitted  8  discontinuously, resulting from solar flare events in the chromosphere. They are  generally  referred to as solar cosmic rays.  Superimposed on the solar contribution is a relatively tenuous omnidirectional flux of higher energy, averaging roughly 2 GeV, wherein some cases individual particle energies have been reported as large as 10" eV! Since the flux originates from outside of the solar system the term galactic cosmic ray has been adopted. In addition, there are compelling arguments favouring an extragalactic origin for individuals possessing energies greater than  10"  eV  (Sreekantan, 1979; Kiraly et al., 1979; Watson, 1980). They are referred to as extragalactic cosmic rays.  The  usual definition of cosmic ray composition  is in terms of charge and energy  spectra. The elemental abundances in cosmic radiation has been extensively reviewed by Cameron (1973) and by Shapiro and Silberberg (1975). Galactic cosmic ray nuclei are primarily protons and alpha particles. In addition to atomic nuclei, galactic cosmic radiation also contains electrons, positrons, and neutral species such as gamma-rays and X-rays. Approximate abundances are given in Table (2.1).  Table 2.1: Composition of Galactic Cosmic Radiation  FAMILY  PARTICLE  ABUNDANCE  Baryons  protons helium nuclei heavier nuclides anti-baryons electrons positrons neutrinos X-rays gamma-rays  ~85% -15%  Leptons Photons  <2%  predicted <l%t detected predicted  t Relative to the proton abundance for E > 1 GeV.  9  In the next section the interaction mechanisms responsible for the production of cosmogenic nuclides are reviewed. We  shall see that these high energy reactions exclude all processes  slower than those determined by the strong force. Consequently, only the baryon component is considered in the cosmogenic nuclide problem. This is mentioned ahead of time in order to 1  avoid a lengthy, and eventually superfluous, discussion of incident leptons and photons. Unlike the galactic flux, the chemical composition of solar cosmic rays is found to vary considerably from flare to flare. The average compostion is roughly 70% protons, 30% alpha particles, and >1%  heavier nuclei. Evidently, the variable nature of both the flux and  the composition of solar cosmic radiation makes it difficult to describe them quantitatively. Moreover, because of the lesser energies involved the effects of solar cosmic rays are restricted to the near surface regions of targets which suffer from the effects of erosion in space (section 2.3). The situation is moie severe for meteorites as they have undergone atmospheric ablation. Consequently, we will be concerned with data taken deep enough in targets (say 100 g-cnr) so that the solar flux can be ignored. Other techniques for filtering 2  out the effects of lower energy particles in the analysis of cosmogenic nuclide data will be discussed in later sections. Similarly; the contribution of possible extragalactic cosmic rays to the production of cosmogenic nuclides is negligible. Although the energy spectrum of the extra-solar flux extends to enormous energies the total energy is insignificant there. This conclusion is further qualified in section 3.3 in a discussion concerned with the energy band limitations of this problem (see Figure 3.6). Thus we have considerably simplified our discussion of cosmic radiation to the baryon component of the galactic flux.  4n section 3.3 we will see that only protons need be considered!  10  Let us now consider the galactic cosmic ray energy spectra for the remaining species of interest Direct flux measurements are influenced by solar modulations (Webber, 1961). It was found that the average flux of galactic particles is roughly 5 nucleons-cm^sec'-sr during 1  solar minimum and about 1 nucleon-cm^sec'-sr  1  during solar maximum. This modulation  becomes progressively less important towards higher energies. For example, the flux of galactic particles with energies greater than 3 GeV is about 1 nudeon-cm^-sec'-sr during solar 1  minimum dropping to roughly half of this value during solar maximum. The attenuation of galactic cosmic radiation throughout the solar system can be of principal concern when studying targets which have fairly eccentric orbits.. However, research into the prehistory of galactic cosmic radiation using the appropriate isotopes cannot generally provide the resolution necessary to detect such orbital effects over the long term (see chapter 4). Clearly, solar modulation introduces a certain degree of uncertainty to the lower end of the galactic cosmic ray energy spectrum (below 1 GeV). Again however, low energy filtering greatly reduces the effect of this problem. There is still the possibility of significant long term solar modulation effects (i.e., changes in solar luminosity). We will address this question again in thefinalchapter. The energy spectra -of galactic cosmic ray protons and helium nuclei are displayed in the right center plot of Figure (2.1). Between 10' and 10 eV/n 15  1  both spectra are effectively  described by a differential power law of the form  S(E) dE = S„E- - dE J  6  The spectra of the heavier elements are similar (see Meyer, 1969).  'Electron volts per nucleon.  (2.1)  11  Log  E  (eV)  Figure 2.1: Some classification and nomenclature commonly used in the description of energetic particles of extraterrestrial origin appear in the left hand figure. A major classification can be established according to whether or not the radiation is of solar origin. The solar flux consists of the solar wind (SW) and the more energetic particles accelerated during solar flare events (F). Some of the latter particles attain cosmic ray energies (SCR). However, negligible amounts are observed with energies greater than about 1 GeV. The differential energy spectra of solar protons and helium nuclei are given in the top right figure (from Fan et al^ 1970). The extra-solar component consists of galactic cosmic rays (GCR) together with a possible contribution from extragalactic sources (EGCR). The differential energy spectrum of the galactic flux is given in the right center figure (Gloeckler and Jokipii, 1967). Note that solar modulation begins to play an important role below 1 GeV. The galactic contribution below 10 MeV in the inner solar system is poorly knowa For completeness the integral energy spectrum of the extra-solar flux above 10 GeV is given in the lower right figure (Meyer, 1980).  12  Equation (2.1) describes the energy spectrum of the galactic cosmic ray flux in space; that is, the spectrum of the primary flux. However, it is the resultant flux within a target, the  so-called secondary flux, which is of concern to the description of cosmogenic nuclide  production. Therefore, we will elicit the necessary empirical observations of galactic cosmic radiation within targets in later sections concerned more with target interactions. Next, let us proceed on to briefly discuss the pertinent facts concerning cosmic ray arrival directions. These observations have been instrumental in providing insight into theories of cosmic ray sources and large scale distributions. However, we are only interested in the solid angle dependence of the galactic radiation so as to provide a complete understanding of "flux" in the forward problem. We  have previously noted that the galactic flux is omnidirectional. One would expect  to detect anisotropies, measured from the inner solar system, on the basis of physical arguments such as i)  the spatial distribution of cosmic ray sources,  ii)  the Compton-Getting effect,  iii)  anisotropies in the interstellar confinement regions, and  iv)  the effects of the interplanetary magnetic field (for lower energies).  1  However, arrival directions are isotropic to within present experimental precision (Cachon, 1962; Elliot et al., 1970). These results apply to particle energies between 10  11  eV and 2 X 10  13  eV.  We must note that these measurements are barely precise enough to detect the net streaming motion of the solar system. The only evidence of extra-solar cosmic ray anisotropies comes from very high energy radiation. Particles with energies in excess of 10' eV tend to arrive preferentially from high 1  •The effect produced from the relative motion of the solar system with respect to the interstellar medium.  13  galactic latitudes (Krasilnikov, 1979). But this is of little concern to the cosmogenic nuclide problem. Thus, let us conclude that the galactic cosmic ray flux is presently omnidirectional and independent of solid angle. However, this may not always have been the case if, for example, the solar system passed very close to large and/or dense interstellar clouds. This completes the discussion concerning those aspects of the primary cosmic ray flux which are essential to the forward problem. In summary, the analysis of cosmogenic nuclide production undertaken in this work elicits a model of the primary incident flux which is characterized as an isotropic omnidirectional flux of galactic cosmic ray baryons possessing a power law energy spectrum with an exponent of -2.6  throughout the applicable range.  This simpie picture becomes inadequate when interest turns to the description of incident high energy radiation within relatively dense matter. The complicated interplay between cosmic ray species and target nuclei at such high energies requires our attention to shift now to the nuclear sciences.  2.2  Pertinent Nuclear Chemistry:  The process by which a nucleus interacts with another nucleus, an elementary particle, or a photon, within a time frame of 10"  12  seconds or less is termed a nuclear reaction. In  such a case the kinetic energies involved are sufficient for the incident particle to enter the nuclear potential well of the target nuclide. Subsequently, it will collide with a target nucleon releasing all kinetic energy into a small volume whose dimensions are prescribed by the strong force (a simple but edifying model developed by Enrico Fermi in 1950). Although the process is ephemeral the strong interaction is assumed to be sufficient to allow the establishment of statistical equilibrium in the volume. Hence, it appears that one can exclude all processes  14 slower than those determined by the strong interaction as noted in section (2.1). Such a process can yield one or more other nuclei, and possibly other particles depending upon the relative energy of the interaction. There are essentially three nuclear reaction mechanisms, classified somewhat arbitrarily according to energy, which have come to be known as i)  compound nuclear reactions (E < 10 MeV),  ii)  direct nuclear reactions (10 < E < 100 MeV), and  iii)  high energy nuclear reactions (E > 100 MeV).  The incident particle of a compound nuclear interaction is completely absorbed by the target nucleus implying that this is inherentiy a low energy process. The lifetime of the resulting excited or compound nucleus is on the order of 10" seconds. However, the transit 16  time of the incident particle across the target nucleus is roughly 10"" seconds and thus the total incident kinetic energy is randomly shared among all nucleons within the system. Moreover, a compound nucleus has no "memory" of how it formed and a succession of particles is emitted from the excited nucleus having relatively low kinetic energies; a process known as evaporation. Unlike the compound nuclear model, the kinetic energy of the incident particle involved in a direct nuclear reaction is not assumed to be randomly distributed among all nucleons within the target nucleus. The time scales are now close to the nuclear transit time and consequently there is "memory" between the incident and final channels. Moreover, there are three types of direct reactions which are generally difficult to distinguish.  1  •Referred to as pickup, stripping, and knockout reactions.  15  Let us now consider the de Broglie wavelength of the incident particle (i.e., the ratio of Planck's constant to the momentum of the particle). At energies of 10 MeV and 100 MeV the particle size (in a quantum mechanical sense) is about 9 fm and 2.8 fm respectively.  1  Thus, the incident particle effectively sees the entire nucleus in the compound and direct reactions. But for higher energies, say 1 GeV and 500 GeV, the nucleus becomes more and more transparent as the de Broglie wavelength of the particle decreases; i.e., 0.7 fm and 0.0025 fm respectively. In fact, at energies above 1 Gev the incident particle interacts with individual nucleons within the target nucleus resulting in a very complicated intranuclear collision process. The resulting outcome of particles has been coined nuclear minestrone. This final class, the high energy reaction, is of principal interest both to the study of cosmic ray nuclei and to the production of cosmogenic nuclides and must be studied greater detail. Consider the interaction between an incident high energy proton and some heavier target nucleus. At high enough energies, the number of particles with which the proton will interact is simply the number of nucleons along the line of sight through the target nucleus. In fact, a reasonable model of high energy nuclear interactions considers the incident proton as executing a random walk inside the nucleus. Hence, Monte Carlo techniques are often applied to calculate the yields of arbitrary nuclides resulting from the interaction. Moreover, any product nuclide can result as long as its atomic mass is below that of the target isotope. In effect, the incident proton chips or spalls nuclear fragments out of the target nucleus, and hence the term spallation. The resulting de-excited nuclide is termed a spallation product. What we have decribed is collectively known as the cascade-evaporation model. An elucidative display of information concerning high energy reactions is the so-called mass yield curve (Figure 2.2). The most striking feature is the broadening of the spectrum at higher energies. In fact, the 3 GeV curve extends over all accessible mass numbers, varying  The fermi (1 fm = 10 cm.) is a unit used frequently for nuclear and elementary particle phenomena. l  u  16  by no greater than an order of magnitude. Evidently, the incident proton has sufficient energy to literally blow the target nucleus apart The 480 MeV curve exhibits two prominent peaks. The first peak, closest to the target, corresponds to the spallation products whereas the next peak, centered at roughly half the atomic mass of the target (lead and bismuth), results from high energyfission.However, the fission mechanism becomes important only for rather high mass targets. Also, notice the formation, in high yield, of very light products during high energy interactions (3 GeV curve). This effect is referred to asfragmentationand again is principally associated with relatively heavy targets. Since the targets of interest to this work do not contain significant amounts offissionableheavy elements and because the energy of the primary radiation is in the GeV range, the principal reaction mechanism of concern to the forward problem is the spallation process.  1  IOOO  1  1  1  1  1  1  1  ;  1  T  4 0 MeV  ,  -  4 8 0 M*V  100  /  \  : -  -la  •E 1  — ' 10  i  -  3000  \  ~  M«V^<^^//  j  -  -  f \ /  nrt ii l 0  I1 20  I1 40  I1 60  1 1 80  I1 100  Ap  I1 120  140  ' I' / 160  L_ 1 1— 180 2O0  Figure 2.2: Mass yield curves are displayed for proton irradiation of heavy target nuclides (lead isotopes and Bi) at three different energy regimes. (From Miller and Hudis, 1959). 309  17  The construction of mass yield curves is naturally based upon knowledge of product yields. The most general quantitative concept describing the probability of a nuclear reaction is that of the cross section o. The probability for a reaction between an impinging particle and a target nucleus can be classically thought of as being proportional to the cross sectional area of the latter and hence is expressed in units of area.  1  V  For a beam of strongly interacting particles incident upon a "thin target" the cross section for a given process, or partial cross section, can be defined from the equation R. = N I a . i  t  i  v  (2.2)  '  where R^. is the number of processes in question occuring per unit mass of target per unit time, N  f  is the number of target nuclei per unit mass, I is the number of incident particles  per unit area and unit time, and area). The  o . is the cross section for the particular process (unit  term thin target formally applies to a body which attenuates the beam only  infinitesimally. On 2  the other hand, one  can  employ "thick targets" for so-called beam  attenuation experiments in which the goal is to determine the total cross section  a  from  the removal of the incident particles from the beam (/.e., attenuation). Such experiments cannot be used to determine partial cross sections that are only a part of the entire interaction. Thin target experiments provide insight into the actual interaction between incident and target species. The results are often referred to as thin target partial cross sections. However, several complications are introduced when considering thick target interactions.  'Note that this description fails for charged particle reactions that must overcome the Coulomb barrier. Nonetheless, the concept of cross section is a useful measure of expressing reaction probabilities. 'Nevertheless, the definition is often massaged to suit the particular information sought  18  Consider a single particle incident upon a target of density p. Clearly, the probability of interaction is directly related to the number of target nuclides in the line of sight which in turn can be related to the target density. For example, a sub-atomic particle passing through 1 centimeter of water "sees" more entities with which it can interact than it would if it were traversing the same distance through air at STP. But if the air path is increased to 8 meters then the total quantity of absorber would be the same as for 1 centimeter of water since the density ratio of water to air at STP is 800. Evidently, one needs to specify both the density and the path length. Thus, the product of these two quantities yields a valid measure of the total mass of absorber traversed, and is referred to as the surface density having the dimensions in cgs units of g-cnr. J  Another important concept involves the product of the number of absorbing centers per unit volume and the effective area (or geometric cross section) of each. Clearly, this is the number of centers encountered by a single incident particle in traversing a unit distance through the target Its reciprocal is defined as the interaction mean free path "l ". Moreover, {  if incident particles still continue onward after a collision with sufficient kinetic energy to strongly interact with more target nuclides then the concept of absorption mean free path, or absorption length "1$comes into play. Plainly, / >/. a  by definition.  As more of the target is encountered more collisions will occur and consequently the relatively low energy flux of high energy interaction debris will increase. Hence, one now must consider a primary and a secondary flux of strongly interacting particles, both of which are depth dependent within the target (see Figure 3.2). It is sometimes convenient to define the empirical concept of thick target cross section which take all of these phenomena into consideration. Otherwise, a thorough quantitative understanding of the radiation throughout the thick target is required when applying thin target yields to estimate the production rate of given nuclides.  19  It would be ideal to possess the partial cross section for every product nuclide resulting for each combination of target isotope, incident particle, and energy of concern to the forward problem being developed in this work. Unfortunately, present experimental results are largely inadequate. Many product species of interest to the study of cosmogenic nuclide production are exceedingly difficult to directly measure (i.e., Be) and further, the energies I0  studied are determined  for the most part by the limitations of current particle accelerators.  More data exists on the partial cross sections of short lived radionuclides since long lived species, which are of key concern to this work, require long and intense bombardments. Absolute  abundances of these species are commonly  determined  by  chemical seperation  techniques or by coincidence counting methods. The lack of precision of the data involved here cannot be overstated. Chemical separation and mass spectrometric analyses are used to determine absolute and  relative abundances respectively of stable products. Data on inert  isotope production is relatively good. However, the multitude of undetermined partial cross sections must be estimated in part by extrapolation into unknown energy regions which elicits an understanding of a further concept. The relation between the variation of a given reaction cross section and the kinetic energy of the interaction is called an excitation /unction. It has been experimentally found that compound nuclear excitation functions (i.e., for low energy interactions) always drop off at higher energies (see Figure 2.3). This is because there is less chance to concentrate more energy on a single particle and hence the probability of the reaction decreases. However, excitation functions for products formed only in high energy interactions are quite different. In particular, high energy excitation functions rise very slowly above the threshold, with an increase of many hundreds of MeV  of bombarding energy before the maximum is reached  (see Figure 2.4). Compare this with the abrupt rise of the low energy excitation functions. Another significant observation of high energy excitation functions is that, after typically levelling off above 1 GeV, they are either virtually constant or exhibit a slight decrease with  Proton Energy (MeV) Figure 2.3: Excitations functions for low energy (compound nuclear) reactions involving proton irradiations of "Cu. From Meadows (1953).  c —  J  1 1M 1  1 1 1 1 1 m i1  III)  :  "Mn 5 — —  ~~—- -  —  1  —  —  ''  4 A  -  / S It u  0.10  —  0.05  0.01 0.005  aooi 0.1  1  1 1 1Mill 0.5 I  1  1 1 1 1 Mil 5 10  1  30  Proton Energy (GeV) Figure 2.4: Excitation functions for the production of "Na, Ai. and Mn based on data from high energy proton irradiation of copper. From Hudis, 1968. 41  1J  21  increasing energy.  It is also important neighboring analyses  to note that  excitation functions for neighboring  products from  targets are nearly identical in shape. This observation has been crucial to previous  concerned with  exposure age determinations  based upon cosmogenic nuclide data (see  Appendix B).  Hence, unknown excitation  functions  particularly  well  partial  cross sections of a given  species require one to extrapolate  beyond  the measurements  made  at attainable  determined  excitation functions  can be used  energies.  to estimate  In addition,  those  of poorly  sampled isotopes by analogies and systematics, and by pertinent calculations based upon nuclear theory. The results of such are known as semi-empirical excitation Junctions.  An bombarded  analytic expression  which  correlates  the yield  data  by protons of energy up to 25 GeV was presented  from  several  by Rudstam  light  targets  et al. (1962),  Rudstam (1966), and by Rudstam and Sorensen (1965). Here, the basic assumptions are that  i)  spallation yields decrease exponentially with decreasing A,  ii)  the relative isobaric yields have a Gaussian distribution centered about the most likely charge and is a smoothly varying functions of A, and  iii)  the production cross section becomes constant at higher energies.  Unfortunately,  this relation  is inapplicable for products which  below that of the target (i.e., A  (  An  improved  version  -  target partial  cross  of this was introduced  by Silberberg and Tsao  mass units  (1973) in  an  a working relation which extended the calculation  sections into new regimes which  cosmogenic nuclides (i.e., Be). In addition, these estimates 10  atomic  = A A > 40).  extension of Rudstam's work. They presented of thin  are forty  are useful to the study of  are more reliable than  previous  ones. The relation is applicable for calculating cross sections for targets in the mass range  22  9<Aj<209 and products in the range 6<A^200 (except for very large or very small values of A A) and has the form  a-*e-«  where 0  0  A  A  ,  e-  B  [  A  P Ou  (2.3)  ,  is the normalizing factor (in millibarns) and the remaining parameters are chosen  according to the given regimes of interest In particular, the first exponential term describes the decrease of cross section as  A A increases, the second exponential term describes the  distribution of cross sections for the production of various isotopes of an element of atomic number Z, and the parameters  Ji and  17  relate to the nuclear structure and the nucleon  pairing respectively. The interested reader is requested to refer to Silberberg and Tsao (1973) for explicit detail concerning this relation as a complete treatment would cover the next few pages of this section. Relative standard deviations could be estimated where actual measured yields were available. They reported values between 20 and 30 percent for 6^Z^<20 at energies above 150 MeV  and. as high as 40 percent for 21^Z^26 above 2 GeV  (note that the assumtion  of constant cross section above threshold is retained here). These estimates are claimed to be more accurate than those based upon both Monte Carlo and previous semi-empirical methods. Hence, one now has an analytic expression describing thin target partial cross sections. We  will see that (2.3) satisfies the yield requirement of the forward problem. Evidently, we  still  require a  sufficient quantitative understanding  concerning the  evolution of particle fluxes when considering thick targets. Naturally, a review of the target, those aspects of which are of immediate concern to the forward problem, must first be addressed. We  will soon see that when interest is focused on the long term irradiation  prehistory then iron meteoroids become the only suitable target  23 2.3  Meteoritic Data and the Fatal Gap:  Of  the various classes of targets currently available for the study of cosmogenic  nuclides only meteorites are of concern to this work. Furthermore, meteorites fall under four 1  broad classifications; namely, i)  chondrites,  ii)  achondrites,  iii)  stoney-irons, and  iv)  irons.  In addition, both chondrites and achondrites are usually referred to as stones. It is thought that these distictions have a genetic significance since it is probable that members of a single class share similar histories. Thus, it is important to establish a set of criteria, in light of the goals of this work, from which to choose from one meteorite class or another. Surprisingly, one important such criterion is based upon meteoroid chronologies inferred from the analysis of cosmogenic nuclides measured in meteorites. As noted in the first chapter the current consensus on interpretations based upon cosmogenic nuclide abundances hold that the galactic cosmic ray flux has been constant to within experimental precision. Thus, one 3  can  easily establish apparent exposure ages of respective  meteorite samples. An  analytic  treatment of such exposure age calculations is presented in Appendix B. The important results of this research are referred to in this work as exposure age histograms (Figure 2.5), the salient features of which are summarized as follows: i)  Cosmic ray exposure ages are very much shorter than the accepted age of the solar system (i.e., ages inferred from the Rb-Sr and Pb-U methods).  A discussion of targets for the analysis of cosmogenic nuclides is given in Appendix C.  J  Recall that this conclusion is justified, for the past 10' years, in Appendix A.  2  • C-Chondrites E E-Chondrites • A-Chondrites 0 Achondrites  O  J-  QJ  XI  •oo no  MYR.  ^Ne-^He/^Ne method  •  Hexahedrites  E3 Fine Octahedrites S Medium Octahedrites •  Course Octahedrites  0  Ataxites  Figure 2.5: Exposure age histograms of nonordinary chondrites (a) and of iron meteorites (b) based upon constant irradiation conditions. The stone exposure ages are based upon 'He content (Zahringer. 1968) whereas the exposure ages of irons are deduced from "Ne content (Wanke. 1966) and from the ratio K/ K (Voshage. 1967). 40  4,  25  ii)  The mean exposure age deduced from iron meteorites ( =>=0.7Gyr) is an order of magnitude larger than that of stoney meteorites.  iii)  All meteorite classes distributions.  iv)  "K- K exposure ages are systematically about 50 percent higher than those based upon the "Ar- Cl, 'Ar- Be, and A T - " A T methods (Voshage and Hintenberger. 1963; Schaeffer et al., 1981).  and sub-classes  exhibit  different  exposure age  40  }t  5  3 ,  10  The latter observation is unequivocal evidence that the respective production rates have not been constant Researchers generally agree upon a multi-collisional model involving more massive parent bodies as the principal account of the various peaked exposure age distributions. In this interpretation the largest peaks signify catastrophic events. Another process that can be used to interpret the exposure age distributions is space erosion. The slow removal of meteoroid surfaces is executed by the action of ion sputtering with the solar wind and by  micTOcratering  via cosmic dust impact at planetary velocities.  Consequently, a sample from an arbitrary depth below the surface of a given meteorite actually resided on the average at a greater depth. This effect conspires to significantly lower the calculated exposure ages (Whipple and Fireman, 1959; Fireman and DeFelice, 1960; Fisher, 1966). Schaeffer et al. (1981) calculated the rate of space erosion on stone and iron meteoroids based upon observations of cosmic dust, meteoroid orbitals, and the cratering record throughout the solar system and upon the results of microcratering experiments. They arrived at erosion rates of 65 cm-Gyr and 2.2 cm-Gyr for stoney and iron meteoroids respectively. l  1  Evidently, space erosion can be neglected in the study of iron meteorites based upon these  conclusions.  26 It is noteworthy that the more competent meteorites are the oldest ones. Plainly, this is also reflected in the conclusions drawn on space erosion rates above. As interest lies with the reinterpretation of the irradiation prehistory, as deciphered from meteoritic data, the exposure ages presented heretofore (i.e., Figure 2.5) cannot be considered for integration into the forward problem developed in this work. However, two important a priori considerations can be retained. Firstly, these results enable one to know the relative order of the exposure ages corresponding to a set of meteorite samples. More important however is the realization that meteorite exposure ages group into well defined clusters. This will have a significant bearing on material of the forthcoming chapter dealing with resolution studies. It is clear from the preceeding discussions that iron meteorites are best suited to provide information on the long term irradiation prehistory. However, there are several other equally strong arguments one can put forth to further bolster this position. Foremost is the fact that iron meteorites possess the simplest target chemistry of all natural thick targets. They are essentially iron-nickel alloys and only contain minute amounts of cobalt, phosphorus, carbon, and sulphur. Moreover, the excitation functions of all pertinent iron and nickel isotopes are nearly identical (see Figure 2.6) so that it suffices to model the bulk composition of most iron meteorites simply by the most abundant such nuclide; namely "Fe. This common assumption of simple target chemistry is adopted in this work. 1  In addition, iron and nickel isotopes are the heaviest common nuclides present in all meteorite classes and consequently are best suited as target nuclides. This is because the range of accessible product nuclides is maximized and because more high energy products (i.e., large  'The discrepancy between assuming an "Fe model to a more accurate compositional model amounts to less than 5% for all samples studied in this work. This is well within the precision associated with experimentally determined yields.  27  Figure 2.6: Excitation functions for the production of K from the four most abundant isotopes found in the iron meteorite Yardymly (Aroos). M refers to "minestrone" (section 2.2). 40  28 AA) are available (recall the discussions on low energy filtering in section 2.1). Furthermore, there is an additional point dealing again with the competent nature of iron meteorites. A meteorite has undergone adverse environmental conditions before reaching the laboratory (i.e., atmospheric ablation and impact). One would expect the destructive effects of such to be less evident for the iron class. Consequently, one has a better idea of the original target geometry during cosmic ray bombardment (see section 3.2). A final point favouring irons is that rare gas losses are least expected from this meteorite class (Imamura et al., 1975). This is an important consideration  since their  interpretation is crucial to the long term irradiation problem. Stable isotopes act as integrators of the flux and consequently are capable of containing information on prehistoric irradiation conditions spanning enormous time scales. This is in contrast to radionuclides, which are a differential effect of cosmic ray interactions, whose temporal limits on possible interpretations are on the order of their respective mean lives. Having said this, it is appropriate to present a survey of cosmogenic species produced in iron meteoroids which are useful to the development of the forward problem. An  account of all radionuclides with half-lives greater than one year found in  meteorites is given in Figure (2.7). Evidently, K is the only radioisotope that lends itself to 40  the long term irradiation problem. The analysis of Be. "Al, and "Cl can only span a few 10  million years within current experimental precision. Hence, the gap in half-life between K 40  and  "Be provides a significant natural barrier to the resolution possible on the long term  irradiation prehistory. This will be fully qualified in chapter 4. We aptly refer to this feature as the "fatal gap" ' in the cosmogenic nuclide problem.  'Adopted in part from comments made by Masatake Honda in a report on contributions to "Session OG 12 A and B" held in Tokyo, Japan in 1979.  16  50  14  12  10 40  o o  129  53  Be  •Mn  26  •Al  60,  36  •CI  41  59 ,  •Ca  Ni  32  • Si  •Ar  63..  •Ni  42 'Ar 22,  55  Na  10  20  . Fe  30  40  50  6 (  i»  ' Co  60  130  Atomic Mass of Products  Figure 2.7: Cosmic ray produced radionuclides with half-lives greater than one year that can be observed in iron meteorites. Note the three order-of-magnitude gap between 53^ and ^^K. This is referred to as the "fatal gap" in this work. Perhaps, useful observations of (in t r i o l i t e inclusions, say) may reduce this gap by an order-of-magnitude.  30 We will restrict the discussion of stable nuclides to the inert gases as they have been most heavily scrutinized upon both in meteorite research and in the determination of spallation yields. In turn, only inert isotopes of low "natural" abundance are considered in this work. We will in fact rely specifically on Ne when attention focuses on modelling the long term n  irradiation prehistory. Finally, let us conclude this discussion on current theories regarding the source(s) of meteorites. We have already noted that knowledge of meteoroid orbits can be of concern to the cosmogenic nuclide problem. Theoretical models are based upon both physical and chemical arguments put forth regarding the condensation of the protostellar accretion disk. In addition, dynamical studies have been used to discount the hypothesis of the planetary origins of meteoroids (i.e., from highly energetic  explosions). However, few direct observations are  available for corroboration. The orbits of three chondrites have been reliably established based upon data obtained from camera networks. They are found to be roughly between 0.7 AU and 5 AU (see Figure 2.8) . Interestingly, both short term comets and the Apollo and Amor asteroids possess similar orbits. The current consensus among researchers of meteoritics hold the most likely origins of meteoroids to be short-period comets and/or the main-belt asteroids. Moreover, Monte Carlo simulations of 34 asteroids in Mars-crossing  orbits suggest that they could be the dominant  source of iron meteoroids encountering the earth (Anders, 1964). Observations of the radial modulation of galactic cosmic rays via the interplanetary magnetic field have been made by spacecraft. In particular, results from Pioneer 10 (Figure 2.9) indicate that this radial modulation is of little consequence to the cosmogenic nuclide problem as developed in this work if one accepts the inferred orbits of iron meteoroids given above.  31  Figure 2.8: Inferred orbits of the three chondrites Pribram (P). Lost City (LC), and Innisfree (I) based upon data from camera networks. In addition, the orbit of an Apollo asteroid and the main-belt asteroids (dotted) are shown. From Sears, 1978.  Pioneer 10  Position  [A.U.]  Figure 2.9: The ratio of galactic cosmic radiation measured at increasing distances from the sun by Pioneer 10 to that measured by IMP 5 (near the earth). From McKibben et al., 1973.  32 In summary, iron meteoroids are the only target suitable to the long term irradiation problem. Moreover, the principal assumptions made are that i)  space erosion is negligible,  ii)  the exposure ages are unknown,  iii)  the target chemistry is simply "Fe, and  iv)  the radial modulation of galactic cosmic radiation in the solar system can be ignored for the orbits of iron meteoroids.  Hence, we have presented an adequate survey of the essentials concerning the forward problem. We nuclide budget  must now translate this into a quantitative  understanding of the cosmogenic  33  3  ANALYTIC STATEMENTS OF THE  One  is now  FORWARD PROBLEM  prepared for a quantitative description of the cosmogenic nuclide budget  within a target meteoroid orbiting through interplanetary space. For generality, the derivations will pertain to radioactive nuclides since stable isotopes constitute the special case where the decay constants vanish in the equations. Consider the production of radioactive nuclides within a target exposed to an arbitrary th  high energy flux of strongly interacting particles. Let n^(t) be the number of the i  species  present at time t per unit mass of target Clearly, the first order rate equation is given as ^ [n.(t)] = P.(t) - X . n.(t)  (3.1)  th  where P .(t) is the i  production rate per unit mass of target at time t and X . is the  associated decay constant The  production  rate is highly uncertain since it depends upon many complex and  poorly understood relationships. In theory, one  must account for different incident particle  species, including secondaries, and possess an accurate description of the isotopic composition of the target Possible time dependence of both the particle flux and energy spectrum must also be considered. In addition, excitation functions and the depth dependence of both particle flux and energy spectrum within thick targets are based upon empirical methods which in turn are largely founded on inadequate data. Finally, assumptions must be made on both space erosion and meteoroid geometry. Understandably, the thick target phenomena significantly contribute to the complexity of this problem. We  shall thus begin with an analysis of thin targets.  34  3.1  Thin Target Production Rates:  The simplest form of the production term is obtained when the target is isotopically pure and when the incident flux is time-invariant, mono-energetic, and consists of a single strongly interacting particle species. Clearly, the thin target assumption must be invoked in order to satisfy the latter point and to neglect depth dependence. In this case, the production term is merely expressed as  P. = N $o. /  where  t  (3.2)  i  is the number of target atoms per kilogram,  (incident particles-nr-sec~') and o.  $  is the omnidirectional flux  is the partial cross section of the \^ species at the  2  energy in question (see Section 2.2). The goal of this paper is to extract information on the cosmic ray flux prehistory. Therefore, one must allow for a time dependent particle flux, 4>(t). Now,  consider an energy spectrum  S(E) over the incident particle flux. If this  distribution is also time-variable then the production term becomes  P/t) = N, *(t) oft)  where oft)  (3.3)  th  is the average partial cross section of the i  species, over the entire energy  range at time t, weighted according to the energy spectrum. That is,  oil)  (3.4)  =  S(E,t) dE  35  Further, if the inddent flux is composed of K particle species and if the target is impure, composed of M th  the i  target isotopes, then one defines o.^  as the partial cross section of  nuclide associated with the inelastic interaction between the k  th  incident species, with  th  respective time dependent energy spectrum S^(E,t), and  the m  target isotope. Then the  mean-target average partial cross section is defined as  M  r°°  M L  t&  =  Yi  = —  m*ikm®  W  p  m a l  <> 15  1 S^E.1) dE  Jo where W  m  is the fraction of the m  sample; that is, defining  th  target isotope averaged over the analysis region of the  as the number of isotopes "m"  per kilogram of target then  N ——  =  (3.6)  W  th  Hence, an expression for the production rate of the i  cosmogenic nuclide in a general thin  target exposed to an omnidirectional particle flux is given as K  P/t) = N, £  tyt)  I.,(t)  k= l  where 4>^(t) is flux of the k'^ strongly interacting incident species. 1  (3.7)  36  3.2  Thick Target Considerations:  Recall the interaction mean free path l  from section (2.2). For a high  t  energy proton  in iron,  10  PFe<We  Consequently, a  hand  specimen  of iron  meteorite  cm.  must  exhibit  the inter-nuclear  cascade  phenomena on a macroscopic scale.  In a discussion of thick target experiments, it is appropriate  to consider  the production  rate as depth dependent since one is dealing with a slab of material exposed to a collimated beam of particles. However, if the incident particle flux is omnidirectional  then the concept of  depth dependence is applicable only to smooth spherically symmetrical targets (this includes the semi-infinite slab as a limiting case). Indeed, if the target is arbitrary in geometry then, if its shape is well known, it is fitting to regard within  me  known then  body since the meaning of depth it is convenient to consider  the production  rate as positionally dependent  is ambiguous here. If the geometry is poorly  surfaces  of constant shielding conditions  within the  target. Clearly, a given shielding condition in such a body can be related to similar shielding effects at an appropriate  depth in a slab exposed to a particle beam (as above). This gives  rise to the concept of effective depth, henceforth denoted by "d".  More specifically, it is both the energy spectrum and primary particle flux which vary within a body. In addition, the cascade particle contribution dependent Hence, a general known geometry is  expression  for the production  to the flux is also positionally  rate within  an arbitrary target of  P/U) = N, £  ^(tgr) Z ^(U)  (3.8)  k=1 where r is the vector relating a given position to the origin of some convenient coordinate system and K'(r) is the number of strongly interacting secondary species, not present in in the primary radiation, as a function of position. In practice, even the basic geometry of an iron meteoroid may not be well known. The  present sample delivery system is violent and does not guarantee recovery of the  complete specimen. It is possible to estimate the original surface profile before atmospheric ablation by mapping concentration contours of a suitable cosmogenic species (see Figure 3.1).  Figure 3.1: Contours of He in a center cross section from the Grant iron meteorite indicate surfaces of constant shielding. In this case the contours indicate that the present shape is similar to the original one. The concentration map is based on mass spectrometric measurements (crosses) in bars cut from the siab. The values indicate content in millionths of a cubic centimeter per gram. (From Reynolds, 1960). 3  38  This is equivalent to mapping surfaces of constant shielding conditions as mentioned earlier. However, the sample must be largely complete and, moreover, such descriptions are nearly absent in the literature. Spherical  geometry is widely  adopted  as  a first order  approximation  for iron  meteoroids. For example, Kohman and Bender (1967) calculated the specific production rate of several nuclides within iron spheres of various radii (see Figure 3.2). They concluded that a comparison of their results with most observations from medium-sized and larger meteorites yields good order-of-magnitude agreement. They also admit, in a comprehensive review of their suppositions, that the spherical assumption "is probably the weakest" since the majority of recovered samples are quite irregular. Hence, it is concluded for this work that current geometrical schemes are inadequate for assigning accurate estimates of shielding effects throughout a given meteorite. One must seek a more indirect method of addressing this problem. Recall that the partial cross sections of various nuclides in a given target, differ in their energy dependence. Hence, a comparison of certain nuclear abundances should provide a sensitive indicator of the effective irradiation hardness which, in turn, can be related to the 1  position within the target The most successful analyses are based upon inert isotope data alone (Signer and Nier, 1960; Voshage and Feldmann, 1978). The depth dependence of particularly useful noble gas species produced from iron spallation is displayed in Figure (3.3). In particular, note the abrupt initial increase in He production. Clearly, this nuclide is made in appreciable yield by 4  the lower energy secondary particles. On  the other hand, Ne J1  exhibits a sharp monotonic  •Irradiation hardness relates to the penetrability of ionizing radiation and is customarily reserved for short wavelength X-rays. In cosmic ray physics the effective irradiation hardness relates to the degree of attenuation in the hard primary component coupled with the development of secondary particles and the associated soft component  Figure 3.2: Calculated specific production rates of a) Be, b) "Al, and c) "CI as a function of depth within iron spheres exposed to the primary cosmic ray flux. Note the initial increase in the first few centimeters. This is where the secondary flux is maximum. (From Kohman and Bender, 1967). l0  D E P T H (cm)  D E P T H (cm)  O  10  20  30  40  50  60  TO  D E P T H (cm)  80  90  100  110  40  decrease indicating that it is a high energy product Hence, the concentration ratio of two such nuclides can serve as an effective irradiation hardness indicator.  TABLE 3.1:  Effective Irradiation Hardness Indicators.  EFFECTIVE IRRADIATION HARDNESSt Ratio  Very Hard Radiat ion ( sha 11 ow t a r g e t s )  He/*He "He/ 'Ne Ar/ 'Ne  0.315 230 4. 05  3  2  38  2  tVoshage  Very Soft R a d i a t i o n (deep t a r g e t s ) 0.235 460 6.4  (1968).  20  40 cm  60  4Tj 6TJ  20 cm  Figure 3.3: Predicted radial variations of [ Ne], [ Ar], [ He], and [ He] in a spherical iron target exposed to the cosmic ray flux. The ordinate is defined so that an infinitesimally small target would yield unit concentration. (From Signer and Nier, 1960). Concentrations are in kilograms. J,  4  3,  3  41  Three such isotopic ratios are given, for both hard and  soft radiation, in Table (3.1).  Evidently, the *He/ Ne ratio is most sensitive to irradiation conditions. This ratio is an 21  integral part of the current K 40  dating technique for iron meteorites as outlined in Appendix  B (Voshage, 1967; 1978). In addition, it is important to note that almost all helium and neon in iron meteoroids is produced by cosmic ray interactions (Buchwald. 1975). Finally, let us examine the factors in equation (3.8). From the previous discussion the general positional dependence should be revised to describe the effective depth dependence so that the factors now  read as *^(t,d) and  main approaches in modelling  production  L.^Ud). Recall from section 2.2 that there are two rates within thick targets. In one  method, the  evolution of the flux and energy spectra are empirically tied into thick target cross sections which are derived from accelerator experiments. When considering cosmic ray primaries natural conditions have to be simulated closely in order to obtain production rates directly (Honda, 1962; Shedlovsky and Rayudu, 1964; Van Ginneken and Turkevich, 1970). Nuclear systematics and  multiple-group  diffusion theory  are used as more indirect techniques of estimation  (Kohman and Bender, 1967; Trivedi and Goel, 1969). Note that the estimates in Figure (3.2) are based upon, the latter analysis. The alternative approach is more allied to-the -physics of the problem and shall be . adopted in this work. In this method, excitation functions (i.e., thin target cross sections) are employed in conjunction with empirical relations describing the evolution of particle fluxes and spectra within thick targets. The spectral relations were determined by comparing the star size distribution - (i.e., nuclear disintegrations) in nuclear emulsions flown at various altitudes in helium balloon experiments (Birnbaum et al., 1952; Powell et al., 1959) and are applicable from 100 to 3000 MeV. For greater energies the spectrum is essentially the same as the primary energy spectrum. In this work a low energy cut-off E^ is forced at . 100 MeV  since the adopted  excitation function (equation 2.3) is inapplicable for lower energies. The consequences will be  42  discussed in the next section. The interested reader should refer to Reedy and Arnold (1972) for an extension of the spectrum to lower energies. Arnold et al. (1961) claimed that the nuclear emulsion results were transferable to iron targets. They calculated the flux and energy spectrum at various depths in iroa Their results are displayed in Figure (3.4). Secondary particles in this energy range are mostly intra-nuclear cascade nucleons together with copious amounts of charged pions. The neutron is the dominant strongly interacting particle below 500 MeV  since most charged particles at lower energies are  strongly impaired by ionization energy losses before interacting with target nuclei.  10  .01  01  02  03  05 ElBeV)  Figure 3.4: The differential energy spectrum at 100 g-cnr in an iron meteoroid as calculated by Arnold et al. (1961) from data provided by Powell et al. (1959). The contributions of protons, neutrons, and charged pions are shown separately along with the total. (From Arnold et al., 1961). 3  43  Empirical relations for the differential energy spectrum  of all strongly interacting  particles were devised for 10 and 100 g-cnr depths (see Table 3.2). Note that no significant J  variation in the energy spectrum is expected beyond the latter depth albeit the total flux diminishes rapidly.  TABLE 3.2:  Energy Spectrum at Two Different Depths Resulting from Incident Cosmic Radiation.t  ENERGY RANGE (GeV) 0.1 - 3.0 >3.0  in Iron  SPECTRUM* 10 g • cm"  depth  2  100 g • cm"  7.2(0.4+E)" -  3.3(0.2+E)" -  1 1 ( l+E) " -  5.8( 1+E)"  2  2  t A r n o l d et a l . (1961). t U n i t s are p a r t i c l e s • cm"  2  2  5  5  depth  2  5  2>5  • s e c " • GeV" . 1  1  An extension of this model to other depths was presented by Reedy and Arnold (1972). They gave the general form of the differential spectrum at some effective depth d as  S(E,d)dE = So(d)[a(d)+E]-"dE  where a determines the shape of the distribution, and S  0  (3.9)  normalizes the expression (as in  Table 3.2). In their model, a decreases with depth as the ratio of soft to hard radiation  44  increases. The (E >  normalizing  constant  is evaluated  from  the  integral  flux  of particles  1 GeV/nucleon) at each depth. The estimated effective depth dependence in these  parameters is shown in Figure (3.5).  Figure 3.5: The parameters for the energy spectrum as a function of depth (equation 3.9). The top curve represents the shape parameter a (d), whereas the bottom curve is the normalizing constant S(d). (From Reedy and Arnold, 1972). 0  As a final note, the spectral index must be modified in light of more recent findings regarding the primary energy spectrum (see Meyer, 1969). More explicitly, the exponent in equation (3.9) should be modified from 2.5 to 2.6 (see equation 2.1).  45  Problems and Assumptions:  3.3  th  Let us recapitulate as follows. The production rate of the i  cosmogenic nuclide at  time t and effective depth d in a thick target, of number density  composed of M  different target isotopes, bombarded by K+K'(d) strongly interacting particle species with respective energy spectra S,(E,t,d) is written as  (3.10)  The immediate problems are that i)  only semi-empirical excitation functions reactions are available, spectra  for high  energy proton-nucleus  ii)  the cosmic-ray-produced available,  of the individual secondary  iii)  the limits of integration are not rigorously established, and  iv)  the time dependence of energy spectra has not been addressed.  species  are not  The obvious consequence of i) and ii) is that all nuclear reactions are treated as high energy proton-nucleus interactions, henceforth referred to as the proton-nucleus assumption. This means that K = l  and K'(d)=0 in equation (3.10). Let us analyse the validity of this forced  simplification before addressing the latter items. To this writer's knowledge, all cosmic ray induced production Z >  rate problems ignore  2 incident primaries since they constitute less than 2% of the total flux. This is  essentially a statement of ignorance concerning  these reactions. In fact, very little is known  even about high energy alpha-nucleus reactions (Silberberg and Tsao, 1973). Those few authors  46  that attempt to include the effects of alpha-nucleus reactions (i.e.. Reedy and Arnold, 1972) are forced to use a phenomenological approach which has little to do with the actual nuclear interaction mechanisms involved. The  important differences between proton-nucleus and alpha-nucleus reactions were  reviewed by Silberberg and Tsao (1973) and are summarized as follows: a)  Reaction mechanisms which contribute to the high peak of (p.pn) reactions at low energies (see Figure 2.3) are inoperative for (a,pn) reactions (Crandall et al., 1956; Lindner and Osborne, 1953; Radin, 1970).  b)  The partial cross sections for lithium and berylium from targets like carbon _ and nitrpgen are enhanced for alpha-nucleus reactions as compared with proton-nucleus reactions (Fonts et al., 1971; Jung et al., 1969).  c)  If one considers the kinetic energy per nucleus rather than per nucleon then the energy dependence of the proton- and helium-induced partial cross sections appear similar (Crespo et al., 1964; Davis et al., 1963; Korteling, 1962; Korteling and Hyde, 1964) albeit the latter are- larger by a factor of two. This is because the energy deposition from proton and helium ion bombardments is similar at the same kinetic enerey per nucleus.  d)  The partial cross sections forAA>3 products in alpha-nucleus reactions at high energies are only 1.6X, rather than 2X larger than in proton-nucleus reactions (Radin, 1970).  The first two items are not pertinent to a discussion of iron spallatioa However, c) strongly supports the proton-nucleus assumption, at least for slightly more massive primariesTTf "one accepts this then the latter point, d), should be considered in the analysis of uncertainties (section 5.2). Similar conclusions can be drawn for pion-nucleus interactions (Orth et al., 1978; Friedlander et al., 1981) and neutron-nucleus interactions (Korteling, 1962; Davis et al., 1963). Hence, the proton-nucleus assumption appears to be justifiable. Let us now  examine problem  iii). High energy cosmogenic nuclide production is  primarily sensitive to a narrow range of the spectrum. This inherent band-limitation is completely specified by the average cross section. The integrand in the numerator of equation  47  (3.5) is the product of two monotonic functions; an increasing excitation function and a decreasing spectral functioa It is displayed in Figure (3.6) for several high energy products at a specific depth. "Al clearly exhibits the expected band limitation for high energy products above E^=100 MeV. The lower limit need only be reduced a few tens of MeV  in order to  obtain similar distributions for the heavier nuclides. The picture is certainly more complicated for "Be, however, since nuclear evaporation supersedes spallation as the principal production mechanism for such light nuclei at lower energies. Nevertheless, the major contribution to the average cross section appears to be well accounted for above 100 MeV. Clearly, one need not be too concerned with energies greater than 10 GeV, particularly in light of the uncertainties accrued thus far. Consequently, an upper limit to the energy can be established. Moreover, only two or so decades of the energy spectrum are of concern to the cosmogenic nuclide budget. Finally, let us examine the latter item iv). One  could invoke various hypothetical  arguments regarding the cause of temporal variations in the cosmic ray flux. Clearly, all such arguments are equally valid in a discussion concerning the possible time dependence of the primary energy spectrum. For it is difficult to imagine a process which can perturb the observed particle "flux by a" ~ common' factor at~ all- energies; -thus leaving—the -shape of -the — entire spectrum unaltered. Indeed, this is practically impossible for cosmic rays since a)  the spectrum spans at least twenty-one decades of energy, and  b)  there are likely to be a host of diverse and uncorrelated sources involved.  However, the previous discussion on the inherent energy filtering of the problem weakens the former point This will prove important after first discussing some pertinent observations. Several independent approaches have been put forth to delineate the spectral prehistory of cosmic rays. For instance, Geiss et al. (1962) obtained a closed solution to their production rate equations which, they claimed, enabled one to deduce the effective energy spectrum over  Figure 3.6: The energy dependence in the production of several important high energy spallation products at 100 g-cm* in "Fe is displayed in the bottom figure. Each of these curves is the product of the energy spectrum at the respective depth (top figure) and corresponding excitation function (centerfigure).Note thatg the excitation functions for "Al. "Q, and K have respectively increasing cross sections for lower energies. This reflects the fact that larger AA products are preferentially produced at higher energies. However, this rule of thumb breaks down for lighter nuclides where nuclear evaporation becomes the dominant production channel from targets like iron. This is exemplified by "Be which is intermediate between Aland "CI. In addition, note that this analysis applied to Ne, a nuclide crucial to delineating information on the long term irradiation prehistory, yields qualitatively similar results to that of "Al as expected. All curves in the lower figure are expected to decline rapidly below 100 MeV. 2  40  62  n  log  E  (MeV)  49 the irradiation history of a given target. This analysis conducted on the Grant iron meteorite 1  suggests that the average energy spectrum above 1 GeV  has been similar to that presently  observed. A fundamentally different approach is based on the analysis of fossil tracks due to cosmic rays in meteorites and lunar samples (Amin  et al., 1969; Bhandari et al., 1971a).  These features can be rendered visible by chemical etching only if the primary ionization of an incident charged particle exceeds a critical value (Fleischer et al., 1967a, b; Lai 1969; Bhandari et al., 1971b, c, d, e; Price et al., 1968; Katz and Kobetich, 1968). This condition is satisfied when the incident particle possesses an appropriate combination of atomic number and velocity. Moreover, the minimum atomic number required for producing etchable tracks in silicates is Z>20 (Lai, 1972). But iron nuclei are the most abundant species above this threshold. Thus, most etchable cosmic ray tracks in stone targets are produced when the kinetic energy of incident iron nuclei drops below a critical value. Clearly, the depth 2  distribution of etchable tracks is a measure of the effective energy spectrum received by a target assuming that a)  the cosmic ray iron flux has always been relatively high,  b)  the iron spectrum is representative of the proton spectrum, and  c)  space erosion can be accounted for.  The conclusion, as one may have surmised, is that the iron energy spectrum averaged over the past few million years is similar to the present spectrum.  •Stauffer and Honda (1962) independently arrived at this result as an empirical correlation relation at about the same time. Refer here for additional details concerning sample analysis. The greatest recordable track length in pyroxenes and olivines is roughly 15 LL corresponding to a critical kinetic energy of 2.5 MeV/n for iron (Lai, 1969). 2  50  Unfortunately, the conclusions put forth from the preceeding discussions provide a false sense of security. From the onset, the reader must have been wary of the potential for cyclic arguments arising from the intimate tie between flux and spectrum. In order to say something quantitative about the spectrum these authors must make suppositions regarding the flux . And, 1  as is typical in cosmogenic research, it is assumed to be constant This is clearly incompatable with the current work. On an intuitive level, however, it appears reasonable that changes in the flux should be more dramatic than variations in the shape of the spectrum over the two decades of energy in question. Of course, our poor understanding  of cosmic ray origin, acceleration  mechanisms, attenuation enroute, etc., make this claim difficult to rigorously defend at present Nonetheless, it is certainly no weaker an assertion than the purely arbitrary claim of constant flux used in long term spectral prehistory investigations. Hence, under this qualitative line of reasoning and  without information to the contrary the weak assumption of spectral time  invariance is adopted. 2  In summary, a tractable version of equation (3.10) has been obtained by considering i)  only proton-nucleus reations and  ii)  a time invariant energy spectrum.  Hence, equation (3.1) can now  be used as the differential equation of the cosmogenic nuclide  budget within an iron meteoroid of known isotopic compositioa Finally, let us extend this analysis to include the spallation product budget of several meteoroids simultaneously. This requires a common origin in time for all samples. Therefore,  •Obviously, the opposite is being done in this work! This conclusion automatically assumes that space erosion is negligible for iron meteoroids (section 2.3) and that spectral variations due to orbital histories within the solar system can be ignored. 2  51  it is necessary to define a time scale with its origin fixed at the present and positive 1  backwards with respect to real time. In addition, let us restrict ourselves to some arbitrarily fixed effective depth d . Thus, the revised and final form of equations (3.1) and (3.10) 0  th  describing the budget of the i  th  cosmogenic nuclide in the j  meteorite is given as  A[V(t,d )] = X. n.(t.d„) - N, «Kt,d ) Z.(d„) 7  0  y  7  0  (3.11)  where equation (3.5) has been modified as  (3.12)  •This assumes that the terrestrial residence times of meteorites are negligible (i.e., for the study of shorter lived isotopes).  52  3.4  Functional Description of Cosmogenic Nu :lide Abundances:  Let us now  engage in a formal discussion concerned with inversion. The linear inverse  problem is defined as one  in which a set of "N"  observables e. is connected to some  unknown model m by a set of linear junctional relationships G.. That is. 1  e. = G/m)  i = l,...N.  (3.13)  Furthermore, the linear problem is assumed to have a special form in which there exists a square integrable function %{\) for each G. such that  e. =  / g/x)m(x)dx  i = l,...N.  (3.14)  •A where / is a real interval. The 2  unknown model m(x)  in (3.14) is additionally square  integrable and in principal should adequately represent the physical system under scrutiny. Moreover, it is clear that the  functions  g/x)  contain  all of the physics  and  assumptions therein, apart from the unknown function m(x), and are henceforth referred to as data kernels (or kernel functions). Clearly, equation (3.14) is an analytic statement of the forward problem. The goal of the inverse problem is centered upon the followinq question: Given (3.14) what can be said about m(x)?  'A functional maps a set of functions into the set of real (or complex) numbers. Note that observables in almost all physical problems are related to the model by an integral transform. In particular, (3.14) is a Fredholm equation of the first kind. 2  53  An important concept which greatly facilitates ones understanding of this question is rooted to the accordance between equations like (3.14) and inner product spaces. Moreover, the analysis of the inverse problem in the Hilbert space framework (i.e., a complete inner product space) yields simple geometric analogues to most of our operations. Within this guise the inverse problem amounts to estimating an unknown vector m from only a few of its components. Most of what follows is based on a series of papers presented by Backus and Gilbert (1967, 1968, 1970). They used this perspective to demonstrate what unique information can be obtained from the finite set of inaccurate data e^. and they showed how one can construct models which reproduce such observations and further, how to contend with the problem of stability therein. Let  us now  reformulate this problem  to comply  with the inversion scheme just  outlined. We seek a linear functional relationship between the measured isotopic abundances in a given set of meteorites and the cosmic ray flux prehistory. Hence, the immediate objective is to transform equation (3.11) into integral form. The procedure begins by introducing an integrating factor %/t)  to equation (3.11).  Clearly, for the single sample case  e/t)  = e  -Xt  (3.15)  and hence  Afn.^d,)] = X.n.(t,d ) 0  -Xt  h.(t,do)] = -e  N^(t,do) Zl(cU)  *N 4> (ido) Z^do) . f  54  Integration over the target exposure time T yields  T  -Xt *(Ldo)dt e  n<0.d) = N , Lfd.) o  (3.16)  where it has been assumed that i)  the initial concentrations (at time T) of the given cosmogenic species are negligible, and  ii) T is well known. Plainly, the more general multir sample case can take the convenient form  (3.17)  th  where H(T. - t) is the Heaviside step function corresponding to the j  sample.  Returning to the nomenclature set out in the beginning of this section one can readily identify (3.17) as the data functional (3.14) through which the data n^0,d) are related to an 7  0  unknown model  4>(Ld ). 0  Clearly, the kernel function  7  g / t , d o ) =  y  N ^ Z / d  0  ) e "  X  t  H ( T . - t )  (3.18)  embodies all the physics, apart from the flux function, and suppositions made thus far. Equation (3.17) is of the precise form  sought in the beginning of this section.  However, there are two computational problems that must be addressed initially. First of all.  55 both sides of (3.17) are immense, when using any standard convention of units, thus abetting numerical instabilities. Secondly, it shall be seen that the success of inversion rests heavily upon the precision of the data kernels. Assuming, for the moment, that the exposure ages are well known then the errors in (3.18) lie almost entirely in the first two factors -fa and L /d ). Normalizing (3.17) by these J  0  factors avoids the latter problem for all intents and purposes albeit the numbers are still unmanageably large. However, the former difficulty can be adequately resolved by an appropriate choice of working units. Henceforth, the form of the data functional and units employed for computational purposes will be as follows:  (3.19) 0  where n/0,d„) -  y  hi z t  e  m(t)  /d„)  j  -Xt  H(T. - t)  * OA)  product nuclides-kg"  1  target nuclides-kg~nm  [Gyr], and  [incident  particles-Gyr' -nm' ]. 1  }  Note that the temporal unit is the gigayear. Of course, all results will be presented in conventional units.  56  RESOLUTION ON THE GALACTIC COSMIC RAY PREHISTORY  What kind of structures can one hope to resolve on the prehistory of galactic cosmic radiation given observed abundances of cosmogenic nuclides? This question is intimately tied to the problem of nonuniqueness in inverse theory and was cleverly addressed by Backus and Gilbert (1968). Let us refer back to the functional description of the • general forward problem; namely, equation (3.14). Suppose one is interested in very localized information concerning the model, say at an arbitrary point x=x<>. In theory, if the kernel function g^. in equation (3.14) is the Dirac function 6(x-x ) then one could recover the model m(x) uniquely at Xo given 0  perfectly accurate data. Realistically however, the best one can achieve is to mimic the Dirac function as closely as possible with an appropriate combination of the data kernels. That is, we form a "pseudo-delta function" lf(x,Xo) by taking linear combinations of the data; i.e.,  5(x,x„) m(x) dx  (4.1)  where  6(x,Xo) =  ^  a(x,) <x). g/  (42)  i  and  where  the coefficients  Q-fXo)  are determined  from  the methods of constrained  optimization. As such, 6^x,Xo) provides a blurred estimate of the model at Xo. The degree of blurring is clearly related to the "closeness" of 5(x,x<,) to the Dirac function. Equation (4.1) provides the only unique information on the model obtainable from a finite set of inaccurate observations since it only depends upon both the coefficients and the data. Clearly, this  57  information is simply weighted averages of m(x) and consequently 5(x,x) is often referred to 0  as an averaging junction.*  Evidently, the width and general form of the averaging functions provide crucial information regarding the resolving power of the data. Hence, they are also referred to as resolving kernels. Unfortunately, the interpretation of averaging functions can be somewhat ambiguous for many problems. This dilemma has been effectively addressed by Oldenburg (1983). However, these problems will prove to be of little consequence to the long term irradiation problem in its present status.  4.1  Derivation of the Resolving Kernels:  Let us now derive the coefficients which satisfy (4.2). The method adopted here is frequently referred to as the first Dirichlet criterion (Oldenburg, 1976). When concerned with accurate data the goal is to minimize the function  /J(x) 0  =  /|5(x.Xo)- 6(x-Xo)| dx J  (4.3)  / 8(x,x)dx = 1  (4.4)  'i subject to the unimodular constraint  /V(x„)  =  0  'l the latter being introduced by Lagrange's method of undetermined multipliers. With this one will attain a set of coefficients which yield the maximum resolution theoretically possible from a given set of data.  'Actually, averaging functions are defined as any unimodular combination of the data kernels.  58  However, all observations are inaccurate. Hence, the averages given by (4.1) must also be inaccurate. Consequently, it becomes necessary to introduce the variance of the average VAR[  into our evolving objective function. In addition, we will adopt the usual statistical assumption of uncorrelated Gaussian errors in order to make the solution tractable. In addition, normalizing both the data and the kernel functions by the respective standard deviations s^. greatly assists in the derivation of resolving kernels. Henceforth in this section, this normalization is so assumed in the notation e. and gix).  Thus, both the data  and the kernel functions are now dimensionless and possess unit variance. Backus and Gilbert (1970) proved that the cost of improved resolution is diminished statistical reliability and vice versa. Therefore, one should  introduce the term describing  measurement accuracy A above into the objective function in accordance with this fact In particular, the coefficients a.  must now be considered as a function of some parameter 6  which governs the trade-off between R and A. 1 We write the objective function as  l//(x<,. 0) = cos6 R(x<>)" + sinQ A(x0) +  2LN(x0)  (4.5)  where L is the Lagrange multiplier. Minimizing with respect to each coefficient a. yields  S(x,x)dx = 0 0  'This leads to the well known "trade-off curves" of Backus and Gilbert (1970).  59  cos 8  a  f  /g/x)gj[x) dx - g <x ) t  0  +  Let us define the matrix  L  j g/x) dx =  0.  T^. to account for the elements generated by the integral in the In addition, let the vector U.  first term of this equatioa . 1  by  -  sine a.  represent  the elements generated  the integral of the last term. Thus, in the more convenient vector notation one can write  cose [a-T-  go] + sine a  - LU = 0  (4.6)  with the unimodular constraint  a-U  Now, values. Since  it becomes  convenient  =  1.  to decompose  (4.7)  the matrix  T  according  to its singular  T is symmetric and positive definite we can always write  T  = R AR  is an orthogonal  containing  the respective singular values. Substituting (4.8) into (4.6) and multiplying by  2  (i.e., Jt  1  R  T  ) and where A  (4.8)  where R  matrix  =  "  T  is a diagonal  yields  'This will later be referred to as the inner product matrix when considering model construction. 'Sometimes referred to as the rotation matrix. See Strang (1980).  matrix R  60 cos0 [ a-R-A - go-R ] + sine a-R - LUR = 0 a  cose [ a - A  - go] + sine a -  U  Ll) = 0.  Defining the diagonal matrix D  = cose A + sin61,  where I is the identity matrix, then the rotated coefficients can be written as  a =• [LU  + cose g ] D . 1  (4.9)  0  Clearly, the unimodular condition (4.7) is invariant under rotation ( i.e., a-U  = a-U  = 1).  Thus, the Lagrange multiplier can be evaluated as  L = [l-cosego-D-'-UMU-D-'-TJ].  Multiplying (4.9) by R  T  places the analysis back into the original unrotated coordinate system.  Hence, the coefficients sought are given as  a(xo.e) = a-R  T  = [ L U + cose go] D ' R . T  (4.10)  61  Finally, the resolving kernels for the cosmogenic nuclide problem, based on the budget of "I" nuclide species analysed in "J" meteorite samples, takes the form J  5(t,U,0) =  where Cland J  I  (4.11)  /  g/t) are given by equations (4.10) and (3.19) respectively. The desired  y  trade-off between accuracy and resolution is governed by 6 . It is usual at this point to construct so called trade-off curves (Backus and Gilbert, 1970) so that a reasonable value of 0  can be assigned However, let us first proceed to discuss the theoretical resolution limit  (i.e^ perfectly accurate data) by setting  0=0.  We  will see that the nature of this problem  does not warrent such an account of data precision.  4.2  Single Sample Analysis:  Let us consider the maximum resolution theoretically possible on the galactic cosmic ray prehistory from cosmogenic nuclide abundances observed in an individual meteorite sample of known exposure age. Only the radionuclides (t,/i =  40  K  (t  1/7  =  1.25  X  10' years),  Be  10  1.6 X 10' years), "AI (t^ = 7.12 X 10 years), and "Cl (t , = 3.1 X 10 years) 5  5  v  are considered here since shorter lived radioisotopes produced in meteoroids (below "Cl) tend to be lower energy products (see Figure 2.7). Furthermore, we will see that adding more than one stable isotope into the analysis is redundant in the absense of uncertainties. In addition, we need not be concerned with the identity of the latter throughout this chapter. The  averaging functions based on these four radioisotopes located at three evenly  spaced positions U are displayed in Figure (4.1) corresponding to exposure ages of 10', 10\ 10*. and 10' years respectively. The most obvious observation is the dramatic loss of  62  Averaging Function  Kernel Function T = 1 0 ° yr  K  resolution  between  Clearly, only  '  40  K  10'  10'  and  has  a response  greater than roughly 2 X 10  7  years. time  years. This  is the source of distinction between the short term problem and the long term problem. The  TV=10 yr  bulk  of  the  short  term  7  averaging functions are well centered over their respective positions albeit significant "side  lobes"  exist  with  some negative  contributions. Nevertheless, they all indicate that the typical resolution is never better than a third of the exposure age intervals given. T =10  yr  On  the other hand, the long term  averaging functions are all essentially the 40  K  data kernel as a consequence of the  fatal gap. Thus, we are now T  0  dealing with  a one data problem Evidently, there is no  hope of recovering any features of the T =10  yr  cosmic  ray model other than general  monotonic trends using this datam alone.  Data kernels and corresponding averaging functions (resolving kernels) based on K, Be, "Al, and 'C1. They are generated at three evenly spaced locations to over four different decades of exposure Figure 4.1: 40  age  10  (arbitrary height).  3  -  63 Further, the addition of a stable isotope (i.e., constant kernel function) cannot ameliorate this situation. A more edifying display of the results generated by equation ( 4 . 1 1 ) is presented in Figure (4.2). Here we have adjacently stacked the resolving kernels with respectively increasing values of U in a perspective view throughout the corresponding exposure age interval. The resulting surface is henceforth referred to as a resolving surface. The relative resolving strength for positions of interest over the exposure age interval becomes immediately apparent  Figure 4.2: Resolving surfaces for exposure ages of IO and 1 0 years respectively based upon K, Be, " A l , and C 1 . 6  40  The  resolving surface corresponding  10  7  3 6  to an exposure age of 1 0 ' years (left figure)  displays two prominent features. Firstly, the diagonal ridge clearly indicates that the resolving kernels are fairly well centered about their respective positions to. Let us refer to this feature as the ridge of resolution. Secondly, the optimal resolving power is apparently associated with  64 the  boundaries of the exposure age interval (i.e., the spikes near grid locations (0,0) and  (T,T) respectively). It is difficult to put forth physical arguments which can reconcile with improved resolution near the initial exposure time. Rather, this probably reflects the advantage of  having precise knowledge concerning the exposure age. We  suggest that any detailed  interpretation of the resolving kernels constructed at the most distant epoch of the irradiation prehistory is dangerous practice. Moreover, the overwhelming problems of determining both precise and accurate exposure age estimates immediately suggests that these features are of little practical consequence. Nevertheless, we leave this as a curiosity of theoretical interest On the other hand, the resolving surface corresponding to an exposure age of 10  7  years (right figure) is nearly void of both features. The height of the resolving kernels near the origin relative to the rest of the interval is striking. Beyond 2 Myrs the functions become broad and moreover the meaning of their respective locations is ambiguous.  There is clearly no need to continue on to the long term problem at this point  For completeness, let us introduce a stable isotope into this analysis. In Figure 4.3 this is done for an exposure age of 10' years. One immediately notices marked changes when comparing to Figure 4.2 (right) albeit the differences are not profound. Clearly, the resolving power has improved near the initial exposure time. Once more, the resolution appears to be optimal around the exposure age boundaries. Consequently, the same argument employed above can be used to mute the apparent interpretive significance of this feature (especially in light of uncertainties). Nevertheless, one is safe in concluding that the addition of another data kernel, a "box car" in this case, can only improve upon the construction of resolving kernels as indicated by Figure (4.3). Unfortunately, the improvement is clearly inadequate here.  Figure 4.3: on K, Be, 40  The  10  Resolving surface for an exposure age " A l , " C l , and a stable isotope.  addition of a stable isotope into me  poorer results. This is due  to the low  based  7  previous example (T=10 -.years) yields even 6  concentration of K  over this relatively small frame of  40  time. Consequently, the decay rate is small and  of 10  hence the  40  K  data kernel mimics that of the  stable isotope. Thus, little is added to the overall resolution.  We  have already noted that  40  K  and  stable isotopes are the only nuclides available to  the long term irradiation problem. Another way kernel  functions  function and  a  span broad  Dirac function! We  the  sufficient  time  of stating this is that only  scale. But  one  cannot  monotonic function (exponential) in a  have just demonstrated this simple fact  way  combine  their respective both  a  constant  that successfully mimics a  66 Hence, we conclude that observations of cosmogenic nuclides from a single meteorite  sample cannot provide localized unique averages with respect to the long term cosmic ray flux prehistory.  4.3  Multi-Sample Analysis:  In any analysis, the introduction of additional independent observations is equivalent to augmenting the amount of information that can become available for interpretation. For example, we demonstrated in the last section that adding a stable isotope into that analysis has a positive albeit minute effect on resolution. Therefore, then one would intuitively expect a marked increase in information from the simultaneous analysis of the said isotopes from a set of meteorite samples of differing exposure ages. In doing so, we have increased the number of data by the factor J which is equal to the number of meteorite samples in the analysis. In particular, the long term problem is now a 2J data problem. Let us arbitrarily begin by reconsidering the analysis represented by Figure 4.2 (left) but now with twice the amount of data introduced via a second meteorite sample (Figure 4.4). In addition, we will assume the exposure age of the new sample to be half that of the former one. Clearly the resolution has significantly improved. For instance, a third spike has been introduced through the additional boundary (center of the plot). Again, the interpretation of this feature strongly depends upon the precision of the shorter exposure age. Furthermore, the ridge of resolution has become more localized by roughly a factor of two. More important however, the resolving kernels are less ambiguous, with respect to the entire interval, than in the previous case as exhibited by the two vanished quadrants.  67  S  Figure 4.4: Resolving -surface based . upon the same radionuclides as per Figure 4.2 (left) but with the addition of data from a second meteorite sample with an exposure age of 5 X 10 years. 5  Let  us  discuss the  kernel is formed by kernels are individual  origin  kernels, derived  two  nil quadrants of Figure  to isotope, the  specimens. For  from  the  two  temporal distance. That is, one  pairing  example, the  resulting  only  respective meteorite  from  2  separate  difference between the analyses,  spans the interval [O.TJ  is their  observations in two  4 0  K  data  respective spans  of  whereas the other spans the interval  [0,T ], where T =2Ti in this example. Therefore, they are identical 2  (4.4). Each resolving  taking linear combinations of the eight data kernels. However, the data  paired according  meteorite  of the  within the interval [O.T,].  68  Hence, when linearly combining these two functions either one can be completely subtracted out in order to localize the resolving function. More explicitely, from equation (4.2),  T(t,U) =  o,g,(t) +  aag»(t)  where g. = e"  M  H(T  - t),  i = l, 2.  Clearly, a resolving kernel centered at t<, e (T,,T] would require that a j = - a 2  the difference of g,(t) and  g (t) vanishes over the region [O.TJ. The 2  2  so that  resulting resolving  function would appear as the shaded portion of Figure (4.5) if only considering the  40  K  observations. One can plainly form resolving kernels in the complementary region [O.TJ in a similar fashion. Hence, one has a complete understanding of the nil regions in Figure (4.4).  T  2  Figure 43: Schematic of two kernel functions based upon the measurements of a given isotopic species (a radionuclide in this example) from two different meteorite samples of respective ages Ti and T . Clearly, they can be linearly combined so that the result vanishes over certain temporal locations. 2  69  What we  have just described has profound consequences. For in theory, one can  obtain the Dirac function simply as  lim 6(U,)  = SO-to).  1  V 2 T  A practical example of such enhanced resolution is displayed in Figure (4.6). Compare this to any previous resolving surface!  Figure 4.6: Averaging surface based upon K and a stable isotope measured in two hypothetical meteorite samples possessing exposure ages of 5 X 10 and 5.5 X 10 years respectively. 40  7  7  •This statement is formally correct if the two data kernels pertain to a stable isotope. Recall that the Dirac function is defined from a unit "box car" whose width vanishes.  70  Evidently, it is more important to know the relative differences of exposure ages than it is to know individual ones accurately. Moreover, parameter errors (i.e., in exposure age) outweigh the importance of data errors. This fact lessens the importance of constructing' trade-off curves (Backus and Gilbert, 1970) at the present time. Recall from section (2.3) that meteorite exposure ages fall into well defined clusters. Thus, our problem is naturally suited to this analysis of resolution. Moreover, this immediately suggests that good resolution on the galactic cosmic ray flux prehistory is generally associated with exposure age clusters. The situation is promising in view of Figure (2.5). Indeed, it is surprising that this analysis only requires measuring a single isotopic species from two separate meteorite samples. Clearly, the choice of cosmogenic species depends upon the most reliable isotopic measurements whereas the choice of meteorite samples is restricted to both the precision (and accuracy to a lesser degree) of respective exposure ages and to the temporal location of interest (which again depends upon exposure age accuracy). Thus, we have established several criteria for limiting the kind of improvements in the data base that are required for a given investigation. In summary, deriving unique averages where sample exposure ages allow provides various smoothed estimates of flux intensities at their respective temporal locations. Hence, one has an indication of flux variations throughout the prehistory. One  could employ current  exposure age determinations (Voshage, 1967, 1978) to choose from respective iron meteorite samples according to their relative age differences. However, the temporal location of these estimates would be uncertain since long term exposure ages are based upon a flux model which is inconsistent with several crucial observations. One can address the long term flux variation problem from a different perspective and simultaneously contend with the uncertainty of the iron exposure ages by now model construction.  turning to  71 5  MODELLING THE LONG TERM IRRADIATION PREHISTORY  Let us finally consider the problem of both modelling the long term galactic cosmic ray  flux prehistory and  of simultaneously recalibrating the iron meteorite exposure age  histogram. Recall the general data functional (3.14). Clearly, there are an infinite number of models m(x) which reproduce a finite set of inaccurate observations e^. (recall than m is an element of a Hilbert space). Further, it is clearly understood that a priori information is largely absent for limiting the possibilities. Hence, we must adopt an objective approach by minimizing key structure^) associated with the model. In particular, since we are refuting the long term constant flux interpretation then it becomes natural to minimize the gradient. Such a model is colloquially referred to as the flattest model and is denoted here by n y Furthermore, the problem is clearly non-linear since the exposure ages are assumed to be unknown. However, the flattest model provides an additional constraint which will prove instrumental in contending with this problem; namely, an initial value m(0). We  will expound  upon this after first formulating the flattest model for the linear problem.  5.1  Derivation of the Flattest Model:  It is usual to apply the methods of variational calculus on the Hilbert space of models in order to seek those which optimize arbitrary criteria. Let us henceforth refer to this space as "model space" and denote it as M. In addition, it is customary to minimize in a least squares sense which implies that M is in fact the real space Lj[a,b] where the norm of the model is defined as  72 Moreover, the data equation (3.14) is simply the inner product of the data kernel and the model. For convenience, let us adopt Dirac's "bra" and "kel" notation whereupon (3.14) and (5.1) become <g|m> and <m|m> respectively. Similarly, a linear vector equation defined by x = Ay is written as |x>=A|y> in this convention. Consider that model which has the smallest norm in M and simultaneously satisfies (4.13). Let us denote this model by m^. This model can be found by minimizing (5.1) subject to the data constraint (equation 3.14) introduced through the Lagrange multipliers L.. That is, we must minimize the objective function  \Jj = <m|m> + 2^~\.[e. - <g |m>].  (5.2)  /  Clearly, ny is that model possessing • the smallest gradient of all models in M. Hence, we must reformulate the data functional (3.14) so that m'(x) takes the place of m(x) in (5.2). This is done by integrating (3.14) by parts to yield - -  f. = m(b)h.(b) - e. = <h.|m>  ;  —  (5.3)  th  where I K is the indefinite integral of the i  data kernel. Thus, the flattest model can be  found by integrating the function which results from minimizing \jj = <m'|m> + 2 ^ \ . [ f . - <h.|m'>]. I  Let us proceed to do this by the method of stationary values.  (5.4)  73  Consider  an  arbitrary  infinitesimal perturbation of the model  6 m'.  Clearly, m' is a  minimum if  \p(m  6m') - l^(m') = 5^(m') =  +  0.  More explicitly,  5l//(m') =  2<m'|  6m'>  <m'  Since  +  -^^^1  L.(-l)<h | 6m'> /  6m'>  =  =  0  (5.5)  0.  6 m' is arbitrary then (5.5) is satisfied for all 6m'. Thus,  m'  where  2  B.  = L.  =7  (5.6)  flh.  are the coefficients which must be determined.  The coefficients are evaluated by substituting (5.6) into (5.3). That is.  f.  <=> where the inner product  matrix  since it is symmetric and  T  positive  =  <h,|  7^  Bh>  |f>=r|/3> has been already defined in section  (4.1). T  definite. Thus, the coefficients are evaluated  is invertable simply  from  the relation  \p>= r-'ifx  (5.7)  74  Hence, the flattest model can be evaluated as  (5.8)  nyt) = Yj.jhfl)dl  + C  where C is the constant of integration. Let us now be explicit in terms of the cosmogenic nuclide problem. The indefinite th  integral of (5.3). pertaining to the i  th  isotopic species measured in the j  meteorite sample,  is evaluated as  X.* 0 i/t) =  A;  e  (5.9)  XT  t - T.  Hence, the new data "T. is given from (5.3) as  (l-e 'T/) - e.. x  'r. =  y  (5.10) $(0)T. -  4..  X. I= 0  and consequently we have introduced the present value of the flux $(0) into the analysis.  75  for Tj>T_ Clearly, replacing the index "j" for "1" in equation (5.11) holds for the case where T>T^.  Notice that the situation where  has not been specified. This is because  the success of invertion heavily depends upon the condition of T. Thus, inversion fails if the two  exposure ages are identical since two  vectors in  T would therefore be linearly  dependent  1  The  condition number of T relates the relative change in the data to the relative  change in the model. This naturally leads into the question of model stability. The usual T according to its singular values. Then,  method of dealing with data errors is to expand one  proceeds to construct a set of orthonormal basis functions from the data kernels  incorporating this expansion. It is found that the smaller singular values are associated with the finer model structure, most of which being statistically unreliable. Thus, the model can be smoothed by winnowing out the smaller singular values based upon some suitable  "misfit''  criterion (i.e., the Chi-squared test). Obviously, the model so described is identical to (5.8) if all singular values are retained. What we have just described is collectively referred to as the spectral decomposition method (Parker, 1977). However, it is clear from (5.8) that model structure is largely dependent upon the collective structure of the data kernels. But only  40  K  and an arbitrary stable isotope are  'Similarly, only one stable isotope can be explicitly introduced into this model. Another way of understanding this is that two identical kernel functions cannot add any more structure to the model than can either one alone.  76 available to the long term irradiation problem. Consequently, one is only capable of generating monotonic long term models given one meteorite sample and its true exposure age. In this case, equation (5.8) will suffice in generating all single sample models of interest to this problem. That is, 1  y[te . x  T  + ^ ( e ' - Dl + X  T  $(0)  A,.*  0 (5.12)  tV2 - Tt +  $(0)  X. =  0.  Furthermore, models based upon the multi-sample analysis can attain structrures whose "wavelengths" are on the order of the respective exposure age differences (section 4.3). These models have been investigated using the spectral decomposition method discussed in section C5.1). In all cases, fine structures are lost when the models are misfit based upon conservative 2  estimates of data errors (section 5.2). Hence, the multi-sample problem will not be pursued in this work.  5.2  Data and Estimates of Uncertainties:  We  have emphasized throughout this work that existing cosmogenic nuclide data and  the respective partial cross sections are largely inadequate. This is reflected in the fact that extensive tabulations of absolute cosmogenic radionuclide abundances do not exist in the literature. Voshage (1967, 1978) has presented exhaustive results of both K 40  and of stable  •However, all model construction in this work is in fact based upon spectral expansion. Hence, this claim has been verified using reasonable estimates of uncertainties (section 5.2). Employing the Chi-squared criterion.  2  nuclide analyses in iron meteorites. Unfortunately, the  40  K  data are only relative concentrations  since the analysis is based upon the mass spectrometer. One  could calibrate these values using  accurate absolute abundance measurements of some well known stable species. Then the data uncertainties would be  largely due  two pertinent yields. However, we  Data  on  to the precision of both  this latter measurement and  will not pursue this method.  absolute abundances of cosmogenic nuclides from  varies greatly throughout  the  the literature. In particular, such data on  specific 40  K  meteorite  samples  is nearly absent as it  is a very difficult species to measure precisely.  On section  the other hand, data on the lighter inert isotopes are relatively good as stated in  (2.2). In particular, "Ne  abundances (and  corresponding  yields  from  known. Moreover, it is well suited since its "natural" abundance is very low is a high  energy  product  with  respect to an  iron target Thus, we  will  iron) are well and  adopt  because it  "Ne  as the  stable nuclide used in the long term irradiation problem.  In  addition, the  terrestrial ages and  samples  multi-sample  analysis.  (1964). The (5.1). Only  of meteorite  samples  should  be  biased  against both  large  multiple exposure ages' as interpretations should be as simple as possible.  Furthermore,  The  choice  must  data adopted  have  experienced  similar  in this work is from  samples which  come closest  cosmic  ray  shielding  the celebrated paper by  to satisfying  half of the original samples were adopted  our  requirements  here. Although  for use  in the  Honda and  Arnold  are  listed  in Table  improved measurements  can be found scattered throughout the literature it is important to restrict our analysis to data from a single source.  'Some meteorites exhibit more than one a. more complicated irradiation history.  exposure age for differing sample locations indicating  78 Table 5.1:  METEORITE ML Ayliff Yardymly± Williamstown Carbo  Data for Use in the Long Term Irradiation Problem.  DATE OF FALL (find) 1959 (find)* (find)  WEIGHT (kg) 013.6 150 031 454  ["Ne]  f  10-» g/g  10-' cmVgt  0.60± 0.02 0.49± 0.03 0.37 ±0.02 0.22± 0.01  8.9 8.15 5.3 3.2  tAt STP. Uncertainties are not available. $Also known as Aroos. • A1 activities indicate short terrestrial age (Honda et al., 1961). J6  This is clearly not an ideal data set As such, it illustrates the severe problems facing current cosmogenic nuclide research. One  should be concerned  about the large scatter in  sample weights as well as the fact that only one meteorite is an observed fall. The latter point can be remedied by observing large activities of shorter-lived radionuclides indicating small terrestrial residence times. However, this information was not obtained for two of the three samples in question. This is not to say that these measurements are nonexistent; one must be well versed in the this literature in order to make such a claim. Again, we stress the need for a compendium of cosmogenic nuclide data. Furthermore, He 4  data was not found and consequently irradiation hardness correlations  among respective samples cannot be made using the methods oulined in section (3.2). Instead, the unorthodox correlation based on He/ Ne has been utilized to establish Table (5.1). This 5  writer is unaware of committing  any  21  "crimes"  in doing so although one  worries when  referring back to Figure (3.3)! For completeness, let us conclude this section with a summary of all the pertinent data and further, present crude estimates of the associated experimental errors. The points just given all indicate that large systematic errors exist in the data. Unfortunately, we have not  79  provided enough information from which to quantify them as such. Quoted precision in Table (5.1) is under 5 percent although a more realistic value may be substantially higher. Recall equation (3.19). According to our formulation both the yield and the target number density values are defined as part of the data. Quoted errors in the latter were not found. On  the other hand, we  discussed the relative standard deviations associated with  individual yield estimates in" section (2.2). However, one must look to Figure 3.6 (bottom) in order to translate yield errors into errors in average partial cross section. Silberberg and Tsao (1973) found the largest errors in equation (2.3) to be associated with energies above 2 GeV for the nuclides of interest Fortunately, the average cross sections all fall dramatically in this energy range in accordance with equation (3.9). Once again however, one can argue about implicit systematic errors as above. Both equation (3.12) and Table (3.2) were employed to evaluate the pertinent average partial cross sections. The respective computing codes were rigorously tested against the data provided in Silberberg and Tsao (1973) and by Arnold et al. (1961). The integration was accomplished by implementing  both spline and numerical integration algorithms (courtesy of  Prof. D. Oldenburg). The necessary steps were taken to assure that accuracy was maintained. The results based - upon the spallation of "Fe are as follows:  Ne  21  4 0  K  5.0 X 10-"  cm,  3.1 X IO"  cm,  27  2  2  Be  7.9 X 10"  cm\  "Al  4.3 X 10-  cm, and  "Q  2.6 X 10-  cm.  10  2  21  27  2  2  Also, the target number density based on "Fe for the accuracy required is  80 N  = 1.1 X 10" kg-'.  Finally, one must possess a value of the present ornnidirectional flux at an effective depth of d = 100 g-cnr. There are two methods of achieving the value investigated in this 1  0  work. Firstly, a freshly fallen meteorite can be analysed for' short-lived radionuclides at the prescribed depth. Assuming secular equilibrium (i.e., XT>>1 and $=constant) over the short term then equation (3.19) becomes A / O . d o V N ^ / d o ) = $(0,do)  (5.13)  where A^.=nV X^. is the \ ^ activity in question and <£(0,d) is the present flux. 0  Equation  (5.13) was evaluated  for radioisotopes observed  in the iron meteorite  Yardymly (Arnold el al., 1961); namely, for Be, "Al, "Cl, "Ti, C, and "Ar. The average 10  14  value obtained is $(0,d) = 10±2 cm"-sec". 1  1  0  The second such approach is based upon integration of an empirical depth dependent cosmic ray spectrum (see Table 3.2 or equation 3.9). The result of 14±2 cnr'-sec" was 1  established over the energy interval E^ = 100 MeV and E  y  = 10 GeV. However, many of  lower energy particles, involved here do hot enter into" the budget of high energy products. Hence this latter figure is likely to be high. We will adopt the former figure. Evidently, the data errors are fairly uncertain although they are clearly significant Thus, a conservative estimate of data error based on the preceeding discussions is on the order of 50 percent; a value typically quoted for uncertainties of results derived from research into cosmogenic nuclides.  81  5.3  Contending with Non-Linearity:  We  now possess both the data and the machinery from which to address the linear  inverse problem. However, equation (3.19) is non-linear since T. is unknown. Our remedy to this apparent impasse is simply an extension of the objectivist philosophy adopted in this work. In particular, we will now consider the flattest model to be a function of the variable 1.. Thus, the goal is to obtain that flattest model m^. which possesses the smallest norm with respect to variable exposure age. That is,  <=>  min<  B.(JJ)\  Y(Tj)\ |3(T.)>, /  VT..  In so doing, we establish a criterion for objectively choosing both an element of model space and a set of corresponding exposure ages. Furthermore, one can impose various degrees of constraint to such choices depending on the number of meteorite samples used in the analysis. Examples of single sample analyses using synthetic data are given in Figures (5.1) and (5.2). They are respectively based upon a constant" flux" model and an exponentially increasing flux model, both spanning 1 Gyr. Both respective Lj-norm plots exhibit subtle differences in 1  character although in general they are similar. For example, the most dramatic increase in the norm occurs while approaching the origin after having passed the global minimum. Intuitively, this is because we are trying to squeeze the "energy" of the true model into an integration time which is less than the exposure age. This is a milestone observation when contending with the multi-sample problem as more than one minimum can occur.  'With respect to real time.  3  TIME  [GYR]  TIME  [GYR]  Figure 5.1: Flattest models generated for five different exposure ages based upon synthetic data (left). The data is generated from a constant flux model and consequently the central curve is the true model. The right figure is a plot of the L,-norm spanning the exposure ages in question.  «v»  TIME  [GYR]  TIME  [GYR]  Figure 5.2: Flattest models generated for five different exposure ages based upon synthetic data (left). The data is generated from an exponential flux model. The right figure is a plot of the Lj-norm spanning the exposure ages in question.  84 Consider the two-sample case. Further, let us generate models using constant flux synthetic data and observe the behavior of the norm (Figure 5.3). Again, the global minimum occurs for the true respective ages since the constant flux model is the flattest possible model. However, notice the strong diagonal ridge. Recall that inversion fails when T, =  T. 2  Hence, this feature is aptly referred to in this work as the ridge of ill-conditionality (with respect to the inner product matrix). Evidently, model construction based upon multi- sample data is best suited to meteorites with largely dissimilar ages. This is in contrast to our results of the resolution studies conducted in section (4.3). The Monte  introduction of more meteorite samples clearly becomes more cumbersome. The  Carlo  approach  could  be  employed  to  sample  sufficiently  the  corresponding  J-dimensional space of model norms in order to establish the global minimum. However, in a cursory investigation of this we  found several nearly identical minima to occur while using  only four hypothetical samples. Clearly, the global minimum norm criterion is ambiguous under certain conditions. It is clear that adequate theory is required before rigorously pursuing the multi-sample data problem. Further, it was  stated in section (5.1) why  models based upon multi-sample data. Thus we  it is currently impractical to construct  shall refrain from any  further discussion  concerning the multi-sample problem. Finally, using only a single datum, an observation of a single isotopic species from an individual meteorite sample, is too unconstrained for this analysis. One can always construct a constant flux model which matches the current flux value by finding the appropriate exposure age (see equation 3.19). Hence, both *°K and "Ne  must be used together in this analysis.  Figure 5.3: Contour plot of the L,-norms of models corresponding to synthetic constant flux data. Here. K and Ne are analysed from two hypothetical meteonte samples (the true ages marked with the cross).  86 Results and Conclusions:  5.4  Let us apply the data from Table (5.1) to equation (5.12) with regards to individual meteorite analyses. The model norms for the ML Ayliff meteorite are displayed in Figure (5.4). This is representative of the other three samples under study. The minimum norm ages of Carbo and Yardymly are systematically about 20 percent lower than those reported by Voshage (1967). Ages for the remaining comparison could be made. The  minimum  two meteorites were determined  norm  ages  but no such  recovered are reported here as follows:  Carbo .....  0.59Gyr  Williamstown  0.67 Gyr  Yardymly  0.76 Gyr  M L Ayliff  0.87 Gyr.  The corresponding models are sampled in Figure (5.5). Moreover, the global flattest models for all four specimens are presented in Figure (5.6). Evidently, all models are in qualitative agreement as to the general increase of the flux with respect to real time. The systematic flattening of the respective models is merely- an artifact of having performed independent inversions of the respective meteoriu'c data, all under the the criterion of global flatness. Various tests for robustness have been administered  (i.e.,  varying the adopted current  flux value about conservative limits) which support this result Hence, we have constructed  models of the galactic cosmic ray flux prehistory, involving recalibrated exposure ages, which are mutually consistent with the respective observations of cosmogenic nuclide abundances. Moreover, the flux appears to have been increasing over the past billion years in accordance with the claim put forth by Schaeffer et al. (1981). Recall that space erosion has  87;  MODEL NORMS  CD  3  3  C CD O  E  CD >  AYLIFF  o  CD  METEORITE  o  o  minimum norm 0.6  0.8  1.0  EXPOSURE AGE  (Gigayears)  Figure 5.4: Model norms based upon K and Ne observations from the iron meteorite ML Ayliff (Arnold and Honda, 1964). The minimum occurs for an exposure age of 870 million years. Figure courtesy of B. Narod. 40  1.2  21  88  2.0  Figure 5.5: Flattest models generated for five different exposure ages based upon K and "Ne data form the iron meteorite ML Ayliff (Arnold and Honda, 1964). The center curve is the flattest possible model which can reproduce these data in the context of this work. Figure courtesy of B. Narod 40  89  SINGLE  METEORITE  INVERSIONS  CARBO WILLIAMSTOWN +  AROOS  ^AYLIFF  *°K.  Ne data from Honda and A r n o l d ,  21  0.3 TIME  0.6  (1964)  1.2  0.9  BP. ( Gigayears)  Figure 5.6: Global flattest models based upon *°K and Ne data form the iron meteorite ML Ayliff (Arnold and Honda, 1964). All exhibit a monotonic increase with respect to real time. Figure courtesy of B. Narod. 21  90 been rejected as a cause for apparent changes in production rates for iron meteorites in section (2.3). In addition, long term changes in solar luminosity are predicted. Consequently, long term solar modulation effects could be used to explain the variation in production rates. However, theoretical studies of stellar evolution suggest that the solar luminosity L has been steadily increasing at an average rate  -^lnL  0.08X10'yr-'  (Newkirk, 1983). Thus, one would expect the galactic flux to be decreasing if there exists a direct relation between solar luminosity and solar modulation (as one may  expect). This is in  contrast to interpretations of cosmogenic nuclide observations. Unfortunately, such a relationship is not presently realized. Thus, it is difficult to elicit local effects which can  conspire to produce time  dependent production rates. Indeed, if the variation is in fact due to changes in the galactic cosmic ray flux then this model provides a vital clue to researchers trying to address the problem of cosmic ray origins. On  the other hand, we  interpretations  are not  required  have demonstrated that drastic changes in exposure age in order to build a mutually consistent  model of the  irradiation prehistory. The conclusions drawn from exposure age histograms are uneffected since the results presented herein only suggest that a calibration error exists regarding the long term ages. Also, it is clear that improvements in experimental precision are essential. However, we have shown how  one can determine what data and associated precision are necessary in order  to address certain problems of interest.  91  Finally, we have clearly outlined where the most serious problems currently exist in the interpretation of cosmogenic nuclide observations. The so-called fatal gap is perhaps the most severe since it is a natural barrier. However, the multi-sample approach may greatly facilitate this situation when the required data precision exists. But the lack of an independent method  for exposure age determinations will always hinder the reliability of all such  interpretations.  92 REFERENCES  Amin, B. S., Lai, D., Lorin, J. C, Pellas, P., Rajin, R. S., Tamhane, A. S., and Venkatavaradan, V. S. (1969). In: Meteorite Research (ed. P. M. Millman). D. Reidel Pub. Co., Dordrecht, pp. 316. Anders, E (1964). Space Sci. Rev., 3:583. Arnold, J. R., Honda, M., and Lai, D. (1961). J. Geophys. Res., 66:3519-3531. Arrol, W. J., Jacobi. R. B., and Paneth, F. A. (1942). Nature, 149:235. Backus, G. E, and Gilbert, F. (1967). Geophys. J. R. Astron. Soc., 13:247-276. Backus, G. E, and Gilbert, F. (1968). Geophys. J. R. Astron. Soc., 16:169^205. Backus, G. E, and Gilbert, F. (1970). Phil."Trans. R. Soc. Land. Ser. A, 266:123-192. Bhandari, N., BhaL S., Lal^D., Rajagopalan, G., Tamhane, A. S., and Venkatavaradan, V. S. (1971a). In: Proc. 2  Ada, Suppl. 2, 3:2611.  Lunar Sci. Conf. (ed. A. A. Levinson), Geochim. Cosmochim.  Bhandari, N., BhaL S., Lai, D., Rajagopalan, G., Tamhane, A. S., and Venkatavaradan, V. S. (1971b). Earth Planet. Sci. Lett., 13:191.  Bhandari, N., BhaL S., Lai, D., Rajagopalan, G., Tamhane, A. S., and Venkatavaradan, V. S. (1971c). Nature, 230:219. Bhandari, N., BhaL S., Lai, D., Rajagopalan, G., Tamhane, A. S., and Venkatavaradan, V. S. (1971d). Nature, 234:543. Bhandari, N., BhaL S., Lai^ D., Rajagopalan, G., Tamhane, A. S„ and Venkatavaradan, V. S. (1971e). In: Proc. 2 Lunar Sci. Conf. (ed. A. A. Levinson), Geochim. Cosmochim. Acta, Suppl. 2, 3:2599.  Bauer, C. A. (1947). Phys. Rev., 72:345. Birnbaum, M., Shapiro, M. M., Stiller, B., and O'Dell, F. W. (1952). Phys. Rev., 86:86-89. Brecher, K_, and Burbidge, G. R. (1972). Ap. J., 174:253-291. Buchwald, V. F. (1975). Handbook of Iron Meteorites. University of California Press. Cachon, A. (1962). Proc. 5^ Inter-American Seminar on Cosmic Rays, 2:39.  Cameron, A. G. W. (1973). Space Sci. Rev., 15:121. Cesarsky, C. J. (1980). Ann. Rev. Astron. Ap., 18:289-319. Crandall, W. E. Millbum, G. P., Pyle, R. V., and Birnbaum, W. (1956). Phys. Rev., 101:329.  93 Crespo, V. P., Alexander, J. M., and Hyde, E It. (1964). Phys. Rev., 131:1765. Davis, R,, Stoenner, R. W., and Schaeffer, O. A. (1963). In: Radioactive Dating, pp. 355- 364. IAEA, Vienna. Ehmann, W.D., and Kohman, T. P. (1958). Geochem. Cosmochim. Ada, 14:340-363. Elliot, H., Thambyapillai, T., and Peacolk, D. S. (1970). Acta Physica Acad. Sci. Hungaricae, Suppl. I, 29:491. Fan, C. Y., Pick, M., Pyle, R., Simpson, J. A., and Smith, D. R. (1968). J. Geophys. Res., 73:1555. Firemann, E L, and DeFelice, J. (1960). / Geophys. Res., 65:3035-3041. Fisher, D. E (1966). F. Geophys. Res., 71:3251-3259. Fleischer, R. L., Price, P. B., Walker, R. M., and Maurette, M. (1967a). J. Geophys. Res., 72:331. Fleischer, R. L., Price, P. B., Walker, R. M., Maurette, M., and Morgan, G., (1967b)./ Geophys. Res., 72:355. Fontes, P., Perron, C, Lestringuez, J., Yion, F., and Bernas, R. (1971). Nucl. Phys., Al65:405. Forbush, S. E (1946). Phys. Rev., 70:771. Friedlander, G., Kennedy, J. W., Macias, E S., and Miller, J. M. (1981). Nuclear and Radiochemistry, 3rd Edition, Wiley-Interscience Publication. Geiss, J., Oeschger, H., and Schwarz, M. (1962). Space Sci. Rev., 1:197-223. Gentner, W., and Zahringer, J. (1957). Geochim. Cosmochim. Acta, 11:60. Gloeckler, G;, and Jokipii, J. R. (1967). Ap. J., 148:L41.  --- -  Honda, M. (1962). /. Geophys. Res., 67:4847. Honda, M., and Arnold, J. R. (1964). Science, 143:203-212. Honda, M., and Arnold, J. R. (1967). In: Handbuch der Physik (ed. S Flugge), vol. XLVI/2. Springer-Verlag, New York. Hudis, J. (1968). 7/7.:Nuclear Chemistry, Vol. 1 (ed. L. Yaffe). Academic Press, New York. Huntley, H. E (1948). Nature 161:356. Imamura, K., Shima, M., and Honda, M. (1915).Earth Planet. Sci. Lett., 26:54-60. Jung, M., Jacquot, C, Baixeras-Aiguabella, C, Schmitt, R,, Braun, H., and Girardin, L (1969). Phys. Rev., 188:1517. Katz, R., and Kobetich, E J. (196$)Phys. Rev., 17(b401.  94 Kiraly, P., Kota, J., Osborne, J. L., Stapley, N. R., and Wolfendale, A. W. (1979). Proc. 16  th  Int. Conf. Cosmic Rays, Kyoto, 4:1-46.  Kirsten, T. A., and Schaeffer, O. A. (1971). /nElernentary Particles; Science, Technology, and Society (ed. L. C. L. Yuan). Academic Press, New York. Kohman, T. P., and Bender, M. L (1967). In: High-Energy Nuclear Reactions in Astrophysics (ed. B. S. P. Shen). W. A. Benjamin Inc., New York. Korteling, R. G. (1962). Ph. D. Thesis, Univ. of California, Berkley; UCRL-10461. Korteling, R. G., and Hyde, E K. (1964). Phys. Rev., 136:3425. Krasilnikov, D. D. (1979). Proc. lrf  h  Int. Conf. Cosmic Rays, Kyoto, 8:26-31.  Lai, D. (\%9).In: Proc. Colloquium on Cosmic Ray Studies in Relation to Recent Developments in Astronomy in Astrophysics (ed. R. R. Daniel). TIFR, Bombay, 1965. Lai, D. (1972). Space Sci. Rev., 14:3-102. Lindner, M., and Osborne, R. N. (1953). Phys. Rev., 91:1501. Longair, M. S. (1981). High Energy Astrophysics. Cambridge University Press. McKibben, R. B., O'Gallacher, J. J., Simpson, J. A., and Juzzolino, A. J. (1973). Ap. JJU:9. Meyer, P. (1969). Ann. Rev. Astron. Ap., 7:1-38. Meyer, P. (1980). In: Origin of Cosmic Rays (ed. G. Setti, G. Spada, and A. W. Wolfendale), IAU Symposium No. 94. London: D. Reidel Publishing Company. Miller, J. M., and Hudis, J. (1959). Ann. Rev. Nucl. Sci., 9:159. Newkirk, G., Jr. (1983). Ann. Rev. Astron. Ap., 21:429-467. Oldenburg, D. W. (1976). Geophys. J. R. Astr. Soc., 44:413-431. Oldenburg, D. W. (1983). /. Geophys. Res., 88:1387-1398. Orth, C. J. (1978). Phys. Rev., C18:1426. Paneth, F. A., Reasbeck, P., and Mayne, K. I. (1952). Parker, R. L. (1977). Ann. Rev. Earth Planet. Sci., 5:35-64. Powell, C. R, Fowler, P. H., and Perkins, D. H. (1959). The Study of Elementary Particles by the Photographic Method. Pergamon Press, New York, p. 442. Geochim. Cosmochim. Acta, 2:300. Price, P. B.. Rajan, R. S.. and Tamhane, A. S. (196%).Ap. J. 151:L109. Radin, J. (1970). Phys. Rev., C2:793. Reasbeck, P., and Mayne. K. I. (1955). Nature, 176:733.  95  Reedy, R. C , and Arnold, J. R. (1972). J. Geophys. Res., 77:537-555. Reynolds, J. H. (1960) Sci. Amer. (November), 203:171-182. Rudstam, G. (1966). Z. Naturforsch., 21a:1027. Rudstam, G., Bruninx, E , and Pappas, A. C. (1962). Phys. Rev^ 126:1852. Rudstam, G., and Sorensen, G. (1966). J. lnorg. Nucl. Chem., 28:771. Schaeffer, O. A. (1962) Ann. Rev. Phys. Chem., 13151-170. Schaeffer, O. A., Nagel, 29:1109-1118.  K., Fechtig,  H.. and Neukum,  G. (1981).  Earth Space Sci.,  Sears, D. W. (1978). The Nature and Origin of Meteorites. Adam Hilger Ltd. Bristol. Shedlovsky. J. P.. and Rayudu, G. V. S. (1964). /. Geophys. Res., 69:2231. Signer, P.. and Nier, A. O. C. (1960). / Geophys. Res., 65:2947-2964. Shapiro, M. M „ and Silberberg, R. (1975). Phil. Trans. Roy. Soc., 277:317. Silberberg, R., and Tsao C. H. (1973). Ap. J. Suppl. Ser., 25:315-333. Sreekantan, B. V. (1979). Proc. 16  th  Int. Conf. Cosmic Rays, Kyoto. 14:345.  Strang, G. (1980). Linear Algebra and its Applications. Academic Press, New York. Tolstikhin, I. N. (1978). In: Terrestrial Rare Gases, Advances in Earth and Planetary Sciences. Center for Acad. Pub. Japan, vol. 3, p. 33-62. Trivedi, B. M. P., and Goel, P. S. (1969). J. Geophys. Res., 74:3909. Twomey7 S! (1977). mtroduction to the Mathematics of "Inversion ~ in Remote Indirect Measurements. Elsevier Scientific Pub. Co., New York.  Sensing  Van  Schus, W. R., and Wood, J. A. (1967). Geochim. Cosmochim. Acta, 31:747-766.  Van  Ginneken, A, and Turkevich, A. (1970).. J. Geophys. Res., 75:5121.  and  Voshage, H. (1967). Z Z. Naturforsch., 22a:477-506. Voshage, H. (1978). Earth Planet Sci. Lett., 40:83-90. Voshage, H., and Feldmann, H. (1978). Earth Planet Sci. Lett., 39:25-36. Voshage, H., and Hintenberger. H. (1963). In: Radioactive Dating, pp. 367-379. IAEA, Vienna. Wanke. H. (1966). Fortschr. Chem. Forsch., 7:322-408. Watson, A. A. (1980). Quart. J. Roy. Astron. Soc., 21:1-13. Webber, W. R. (1961). Prog. Elementary Particle Cosmic Ray Phys., 6:77ff.  Whipple, F. L, and Fireman, E L (1959). Nature, 183:1315. Zahringer, J. (1968). Geochim. Cosmochim. Acta, 32:209-237.  97  APPENDIX A:  Previous Inferences Drawn on the Cosmic Ray Flux Prehistory  Let us describe the reasoning which has led to the current model of the short term galactic cosmic ray flux (over the past 10 years). The theme has been centered upon 6  comparing predicted production rates to ones calculated from cosmic ray produced radionuclides spanning 10  4  years in half-life (Figure 2.7) from the same sample of meteorite. The th  production rate of the i  radioisotope in pure iron can be written as  (A-1)  E where all symbols are described in chapter 3. On the other hand, the respective decay rate, or activity A., measured at the end of irradiation period T (i.e., at t=0) is  (A-2) o (see equation 3.16). In particle accelerator research the irradiation conditions are usually held constant. Consequently, - after a given time the condition 7>>l/\.  applies. This is always the case for  all isotopes except for K. found in iron meteorites (compare Figures 2.5 and 2.7). Thus, 40  equation (A-2) now reads as  A/d) =  a condition referred to as secular equilibrium.  ?fd)  (A-3)  98 Logically, the only inference that can be drawn from observed activities then is to say that the irradiation conditions have not been constant if condition (A-3) fails. However, this 1  analysis conducted on freshly fallen meteorites supports condition (A-3) (i.e., Arnold et al., 1961) and it has been customary to assume that the galactic cosmic ray flux has been constant to within experimental precision (by about a factor of two). Of course, the problem is that a constant flux model is only one of an infinite set of models which reproduce this finite set of real observations. Nonetheless, this model is acceptable when one acknowledges the lack of contradictory information. The minimum structure model must be given favour above all others for the sake of objective interpretation. This is the same reasoning which has led to the flattest model formulation contained in this work. Since Be is the longest lived radionuclide to which this analysis can be applied then I0  the inference of constant irradiation conditions holds for a temporal span on the order of its half-life; namely, 10 years. 6  Assuming that (A-l) is evaluated correctly.  99. APPENDIX B:  Exposure Age Calculations Based Upon Constant Irradiation Conditions  All cosmic ray exposure age calculations are based upon constant irradiation conditions. Further, the analysis requires two cosmogenic species, a radionuclide which provides a measure of the flux (i.e., assuming secular equilibrium) and a stable species which serves as an integrator of the flux. From equation (3.16) the abundance of a stable species n^ produced under constant irradiation conditions after a time T is  (B-l)  n^O.d) = N a(E)$(d,E)T t  where all symbols and the time scale are defined in chapter 3. Similarly, the abundance of radionuclides n is r  n(0,d) = N a (E)$(d^)[l-e r  If T>>l/X  f  xt  r  ]/ \  r  then the activity may be written as  A/O.d) =  a(E)$(d,E)  (B-2)  The ratio of (B-l) and (B-2) yields the basic expression for the exposure age as  T = Rn^(0,d)/A(0,d) r  (B-3)  where R is the ratio of radioisotope yield to stable product yield. Clearly, the energy dependence of the respective reaction cross sections is assumed to be identical. Hence, the  100  nuclides are chosen to be either isobaric or isotopes of the same element so that this simplification holds. Many variations of equation (B-3) exist throughout the literature. Most notable is that of Voshage (1967, 1978) for the analysis of iron meteorites. It is based upon the radionuclide 40  K  and the stable species K. 41  Note that K 40  In addition, an additional stable isotope K 3,  is not in secular equilibrium since T *^ /  1/X.  is introduced empirically to establish the effective  depth d. However, systematic discrepancies exist among ages determined from Voshage and those based upon shorter-lived isotopes. Thus, the assumption of constant irradiation conditions must be incorrect and consequently one expects the exposure age estimates of meteorites to become progressively more inaccurate with increasing exposure age.  101  APPENDIX C:  A Survey of Targets for the Study of Cosmogenic Nuclides  The study of cosmogenic nuclides is confined to those targets which can be analysed in the laboratory. Presently, we have the following kinds of targets available for radiochemical and mass spectrometric analyses: a)  the upper atmosphere,  b)  meteorites,  c)  cosmic dust,  d)  the lunar surface,  e)  high altitude balloon payloads, and  f)  retrieved spacecraft  Perhaps the best known example of cosmic ray interaction with  matter is  the  production of C from the reaction N(n,p) C in the stratosphere and upper troposphere. 14  ,4  14  However, long lived or stable nuclides produced in the earth's atmosphere will be transported away from their point of origin and perhaps undergo various geochemical reactions, all of which are not quantitatively well understood Consequently, the terrestrial cosmic ray fossil record is extremely difficult to decipher. Cosmic dust could be useful for the analysis of thin target interactions by cosmic radiation. However, the chemical composition of cosmic dust is still not clearly understood and is usually difficult to distinguish from terrestrial dust. Moreover, sufficient sample weights are currently unobtainable  for the detection of radionuclides except for reservoirs on the earth  which unfortunately are plagued with terrestrial contamination.  10  On the other hand, targets carried aloft in high altitude (helium) balloon payloads and targets in the form of retrievable spacecraft have both a well known chemical composition and a well known history of irradiation. The former are particularly useful for direct short term flux measurements and for the determination  of empirical relationships describing the  cosmic ray thick target energy spectrum (see section 3.2). The latter has been particularly useful for studying the effects caused by the geomagnetic field but has little to do with the galactic cosmic ray flux. One exception is the Surveyor 3 spacecraft which resided on the lunar surface for two and a half years prior to retrieval, in part, by the Apollo 12 astronauts. In order to examine the effects of galactic cosmic radiation over longer time scales one must turn to lunar surface samples and to meteorites. Lunar samples afford the advantage of having a well known location within the solar system in contrast to meteoroids whose orbits are poorly understood. The analysis of cosmogenic nuclides from deep lunar core 1  samples yields information on the lunar irradiation prehistory involving galactic cosmic radiation which in turn involves both the galactic cosmic ray flux prehistory and the stratigraphic evolution of the sampled selenographic complicated  region. Clearly, the latter constitutes a significantly  target prehistory. Moreover, lunar material has a relatively complicated 2  target  chemistry. The fact that data concerning product yields from a wide variety of target nuclides is both sparse and imprecise (section 2.2) clearly makes the simplest targets most attractive. The discussion of meteoroids is of principal interest to this paper and the discussion of such is given in section (2.3).  'However, this is probably not too important since the orbits are known not to be eccentric enough to sample significant variations in the galactic flux as a consequence of solar modulation within current experimental precision. Besides, such effects would average when considering the long term problem. But one can argue' that good independent observations are available for constraining the possible interpretations (i.e., impact craters,- estimated influx of cosmic dust, etc.). J  

Cite

Citation Scheme:

        

Citations by CSL (citeproc-js)

Usage Statistics

Share

Embed

Customize your widget with the following options, then copy and paste the code below into the HTML of your page to embed this item in your website.
                        
                            <div id="ubcOpenCollectionsWidgetDisplay">
                            <script id="ubcOpenCollectionsWidget"
                            src="{[{embed.src}]}"
                            data-item="{[{embed.item}]}"
                            data-collection="{[{embed.collection}]}"
                            data-metadata="{[{embed.showMetadata}]}"
                            data-width="{[{embed.width}]}"
                            async >
                            </script>
                            </div>
                        
                    
IIIF logo Our image viewer uses the IIIF 2.0 standard. To load this item in other compatible viewers, use this url:
http://iiif.library.ubc.ca/presentation/dsp.831.1-0085783/manifest

Comment

Related Items