Published March 11, 1998
| Accepted Version + Published
Journal Article
Open
Stellar forensics — II. Millisecond pulsar binaries
- Creators
-
Hansen, Brad M. S.
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Phinney, E. Sterl
Chicago
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Abstract
We use the grid of models described in Paper I to analyse those millisecond pulsar binaries whose secondaries have been studied optically. In particular, we find cooling ages for these binary systems that range from < 1 to ∼15 Gyr. Comparison of cooling ages and characteristic spin-down ages allows us to constrain the initial spin periods and spin-up histories for individual systems, showing that at least some millisecond pulsars had sub-Eddington accretion rates and long magnetic field decay times.
Additional Information
© 1998 RAS. Accepted 1997 October 14. Received 1997 May 30; in original form 1996 November 25. The authors thank Marten van Kerwijk for use of results prior to publication and discussion of white dwarf observational uncertainties, and Glenn Soberman for discussions about mass transfer in binaries, as well as the referee, Frank Verbunt, whose comments contributed greatly to the clarity of this paper. This work was supported by NSF grant AST93-15455 and NASA grant NAG5-2756.Attached Files
Published - Hansen_et_al-1998-Monthly_Notices_of_the_Royal_Astronomical_Societyb.pdf
Accepted Version - 9708274.pdf
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Additional details
- Eprint ID
- 92688
- Resolver ID
- CaltechAUTHORS:20190205-142100054
- NSF
- AST 93-15455
- NASA
- NAG5-2756
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2019-02-05Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field
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