期刊
ASTROPHYSICAL JOURNAL
卷 722, 期 2, 页码 1030-1034出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/722/2/1030
关键词
binaries: close; gravitation; pulsars: individual (PSR B1913+16); stars: kinematics and dynamics
资金
- US National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [0807556] Funding Source: National Science Foundation
- Office Of The Director
- Office Of Internatl Science &Engineering [0968296] Funding Source: National Science Foundation
We present results of more than three decades of timing measurements of the first known binary pulsar, PSR B1913+16. Like most other pulsars, its rotational behavior over such long timescales is significantly affected by small-scale irregularities not explicitly accounted for in a deterministic model. Nevertheless, the physically important astrometric, spin, and orbital parameters are well determined and well decoupled from the timing noise. We have determined a significant result for proper motion, mu(alpha) = -1.43 +/- 0.13, mu(delta) = -0.70 +/- 0.13 mas yr(-1). The pulsar exhibited a small timing glitch in 2003 May, with Delta f / f = 3.7 x 10(-11), and a smaller timing peculiarity in mid-1992. A relativistic solution for orbital parameters yields improved mass estimates for the pulsar and its companion, m(1) = 1.4398 +/- 0.0002 M(circle dot) and m(2) = 1.3886 +/- 0.0002 M(circle dot). The system's orbital period has been decreasing at a rate 0.997 +/- 0.002 times that predicted as a result of gravitational radiation damping in general relativity. As we have shown before, this result provides conclusive evidence for the existence of gravitational radiation as predicted by Einstein's theory.
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