Статья

Precision Timing of PSR J0437−4715: An Accurate Pulsar Distance, a High Pulsar Mass, and a Limit on the Variation of Newton’s Gravitational Constant

J. P. W. VerbiestAustralia Telescope National Facility-CSIRO, P.O. Box 76, Epping, NSW 1710, AustraliaM. BailesCentre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218 Hawthorn, VIC 3122, AustraliaW. van StratenCentre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218 Hawthorn, VIC 3122, AustraliaG. B. HobbsAustralia Telescope National Facility-CSIRO, P.O. Box 76, Epping, NSW 1710, AustraliaR. T. EdwardsAustralia Telescope National Facility-CSIRO, P.O. Box 76, Epping, NSW 1710, AustraliaR. N. ManchesterAustralia Telescope National Facility-CSIRO, P.O. Box 76, Epping, NSW 1710, AustraliaN. D. R. BhatCentre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218 Hawthorn, VIC 3122, AustraliaJ. M. SarkissianAustralia Telescope National Facility-CSIRO, P.O. Box 76, Epping, NSW 1710, AustraliaB. A. JacobyNaval Research Laboratory, 4555 Overlook Avenue SW, Washington, DC 20375S. R. KulkarniRobinson Laboratory, California Institute of Technology, Mail Code 105-24, Caltech Optical Observatories, Pasadena, CA 91125

2008en

ABI

Аннотация

Analysis of 10 years of high-precision timing data on the millisecond pulsar PSR J0437–4715 has resulted in a model-independent kinematic distance based on an apparent orbital period derivative, P_b, determined at the 1.5% level of precision (D_k = 157.0 ± 2.4 pc), making it one of the most accurate stellar distance estimates published to date. The discrepancy between this measurement and a previously published parallax distance estimate is attributed to errors in the DE200 solar system ephemerides. The precise measurement of P_b allows a limit on the variation of Newton's gravitational constant, |G/G| ≤ 23 × 10^−12 yr^−1. We also constrain any anomalous acceleration along the line of sight to the pulsar to |a⊙/c| ≤ 1.5 × 10^−18 s^−1 at 95% confidence, and derive a pulsar mass, m_(psr) = 1.76 ± 0.20 M⊙, one of the highest estimates so far obtained.\n

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Идентификаторы

DOI: 10.1086/529576

Цитирования и источники

Цитирований: 2Использованных источников: 0

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