Journal
ASTROPHYSICAL JOURNAL
Volume 711, Issue 2, Pages 764-771Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/711/2/764
Keywords
binaries: general; pulsars: general; pulsars: individual (PSR J1802-2124); stars: evolution
Categories
Funding
- UBC UGF
- ATNF
- Swinburne University of Technology Visiting Distinguished Researcher Scheme
- NSERC
- US NSF [AST 9987278, 0206044, AST 0647820]
- WVEPSCoR
- CSIRO
- Region Centre in France
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [0807512, 0206044] Funding Source: National Science Foundation
- Science and Technology Facilities Council [ST/G002487/1] Funding Source: researchfish
- STFC [ST/G002487/1] Funding Source: UKRI
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PSR J1802-2124 is a 12.6 ms pulsar in a 16.8 hr binary orbit with a relatively massive white dwarf (WD) companion. These properties make it a member of the intermediate-mass class of binary pulsar (IMBP) systems. We have been timing this pulsar since its discovery in 2002. Concentrated observations at the Green Bank Telescope, augmented with data from the Parkes and Nancay observatories, have allowed us to determine the general relativistic Shapiro delay. This has yielded pulsar and WD mass measurements of 1.24 +/- 0.11 M-circle dot and 0.78 +/- 0.04 M-circle dot (68% confidence), respectively. The low mass of the pulsar, the high mass of the WD companion, the short orbital period, and the pulsar spin period may be explained by the system having gone through a common-envelope phase in its evolution. We argue that selection effects may contribute to the relatively small number of known IMBPs.
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