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首页> 外文期刊>The Astrophysical journal >PROBING THE MASSES OF THE PSR J0621 + 1002 BINARY SYSTEM THROUGH RELATIVISTIC APSIDAL MOTION
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PROBING THE MASSES OF THE PSR J0621 + 1002 BINARY SYSTEM THROUGH RELATIVISTIC APSIDAL MOTION

机译：通过相对应的寄生运动探究PSR J0621 + 1002二元系统的质量

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摘要

Orbital, spin, and astrometric parameters of the millisecond pulsar PSR J0621 + 1002 have been determined through six years of timing observations at three radio telescopes. The chief result is a measurement of the rate of periastron advance, ω= 0°.0116 +- 0°.0008 yr~(-1). Interpreted as a general relativistic effect, this implies the sum of the pulsar mass, m_1, and the companion mass, m_2, to be M = m_1 + m_2 = 2.81 +- 0.30 solar mass. The Keplerian parameters rule out certain combinations of m_1 and m_2, as does the nondetection of Shapiro delay in the pulse arrival times. These constraints, together with the assumption that the companion is a white dwarf, lead to the 68% confidence maximum likelihood values of m_1 = 1.70_(-0.29)~(+0.27) solar mass and m_2= 0.97_(-0.15)~(+0.27) solar mass and to the 95% confidence maximum likelihood values of m_1 = 1.70_(-0.63)~(+0.59) solar mass and m_2 =0.97_(-0.24)~(+0.43) solar mass. The other major finding is that the pulsar experiences dramatic variability in its dispersion measure (DM), with gradients as steep as 0.013 pc cm~(-3) yr~(-1). A structure function analysis of the DM variations uncovers spatial fluctuations in the interstellar electron density that cannot be fitted to a single power law, unlike the Kolmo-gorov turbulent spectrum that has been seen in the direction of other pulsars. Other results from the timing analysis include the first measurements of the pulsar's proper motion, μ = 3.5 +- 0.3 mas yr~(-1), and of its spin-down rate, dP/dt = 4.7 x 10~(-20), which, when corrected for kinematic biases and combined with the pulse period, P = 28.8 ms, gives a characteristic age of 1.1 x 10~(10) yr and a surface magnetic field strength of 1.2 x 10~9G.
机译：毫秒脉冲星PSR J0621 + 1002的轨道，自旋和天文参数已通过在三台射电望远镜中进行的六年时间观测确定。主要结果是测量周质推进速率ω= 0°.0116 +-0°.0008 yr〜（-1）。作为一般相对论效应，这意味着脉冲星质量m_1和伴随质量m_2的总和为M = m_1 + m_2 = 2.81 +-0.30太阳质量。开普勒参数排除了m_1和m_2的某些组合，未检测到脉冲到达时间中的Shapiro延迟也是如此。这些约束以及同伴是白矮星的假设，导致m_1 = 1.70 _（-0.29）〜（+0.27）太阳质量和m_2 = 0.97 _（-0.15）〜的68％置信最大似然值。 （+0.27）太阳质量和m_1 = 1.70 _（-0.63）〜（+0.59）太阳质量和m_2 = 0.97 _（-0.24）〜（+0.43）太阳质量的95％置信最大似然值。另一个主要发现是脉冲星在其色散量度（DM）中经历了巨大的变化，其梯度高达0.013 pc cm〜（-3）yr〜（-1）。对DM变化的结构函数分析揭示了星际电子密度中的空间波动，该空间波动无法适应单个幂律，这与在其他脉冲星方向上看到的Kolmo-gorov湍流谱不同。时序分析的其他结果包括对脉冲星正常运动的首次测量结果，μ= 3.5 +-0.3 mas yr〜（-1），其下降速率dP / dt = 4.7 x 10〜（-20） ，经校正运动学偏差并与脉冲周期结合，P = 28.8 ms，给出的特征年龄为1.1 x 10〜（10）yr，表面磁场强度为1.2 x 10〜9G。

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