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Mass and geometric measurements of binary radio pulsars

University of British Columbia

One of the primary, long-term goals in high-energy astrophysics is the measurement of macroscopic parameters that constrain the equation of state for compact stellar objects. For neutron stars, known to be composed of the densest matter in the Universe, measurements of their masses and sizes are of considerable importance due to the poorly understood processes that govern their interiors. Measurements of relativistic “post-Keplerian” effects in binary systems can be used to significantly constrain viable equations of state, test modern theories of gravitation, verify binary-evolution models that predict correlations between certain binary parameters, and determine the Galactic neutron-star mass distribution that is expected to reflect different supernovae mechanisms and evolutionary paths. In this thesis, we use established pulsar-timing techniques to analyze signals from radio pulsars in 25 binary systems, as well as from one pulsar in a hierarchical triple system, in order to detect perturbations from Keplerian motion of the bodies. We characterize observed relativistic Shapiro timing delays to derive estimates of the component masses and inclination angles in 14 pulsar-binary systems, and measure a large number of secular variations due to kinematic, relativistic and/or third-body effects in the majority of binary systems studied here. We find a wide range of statistically-significant pulsar masses and make new detections of the relativistic Shapiro-delay signal in four binary systems for the first time. In the relativistic PSR B1534+12 binary system, we derive an accurate and precise rate of geodetic precession of the pulsar-spin axis -- due to secular variations of electromagnetic pulse structure -- that is consistent with the prediction from general relativity. In the PSR B1620-26 triple system, we discuss ongoing efforts to simultaneously model both “inner” and “outer” orbits and tentatively measure secular variations of all “inner-orbital” elements that we show are likely due to third-body interactions between the smaller orbit and outer companion, which can eventually be used to constrain orientation angles and possibly the pulsar mass in the near future.

Text

2016-11-02

Attribution-NonCommercial-NoDerivatives 4.0 International

http://hdl.handle.net/2429/59597

Astronomy

University of British Columbia

UBCV

http://creativecommons.org/licenses/by-nc-nd/4.0/