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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 ,
Eric M. Splaver  and
Ingrid H. Stairs
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

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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 (m2/m1 ≪ 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
Information
Symposium - International Astronomical Union , Volume 218: Young Neutrons Stars and their Environments , 2004 , pp. 49 - 52
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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