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Heavy Neutron Stars? A Status Report on Arecibo Timing of Four Pulsar – White Dwarf Systems

Published online by Cambridge University Press:  19 July 2016

David J. Nice
Affiliation:
Physics Department, Princeton University Box 708, Princeton, NJ 08544 USA
Eric M. Splaver
Affiliation:
Physics Department, Princeton University Box 708, Princeton, NJ 08544 USA
Ingrid H. Stairs
Affiliation:
Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada

Abstract

Relativistic phenomena (orbital precession, Shapiro delay, and/or orbital decay) have been measured in Arecibo timing observations of four pulsar-white dwarf binaries, leading to constraints on the neutron star masses. We have detected the decay of the PSR J0751+1807 orbit due to gravitational radiation emission, the first such measurement in a binary with a low mass ratio (m 2/m 1 ≪ 1). Timing data constrains the mass of this pulsar to bet between 1.6 and 2.8 M. Masses of the other pulsars are in marginal agreement with the canonical pulsar mass of 1.35 M, but higher values are preferred.

Type
Part 1: Neutron Star Formation and Evolution
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

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Heavy Neutron Stars? A Status Report on Arecibo Timing of Four Pulsar – White Dwarf Systems
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