论文标题
中等回收的脉冲星二进制中的相对论效应：PSR J1952+2630
Relativistic effects in a mildly recycled pulsar binary: PSR J1952+2630
论文作者
论文摘要
我们报告了PSR J1952+2630的定时观测结果，轨道上有20.7毫秒的Pulsar，具有巨大的白矮人伴侣。随着计时基线的增加，我们获得了该系统的天体，自旋和二元参数的改进估计值。我们在适当的运动上获得了一个数量级的改进，并且首次检测到该系统中的三个凯伯利亚后参数：Periastron的前进，轨道衰变和夏皮罗延迟。我们将PULSAR质量限制为1.20 $^{+0.28} _ { - 0.29} \ rm m _ {\ odot} $及其同伴的质量为0.97 $^{+0.16} _ { - 0.13} \ 0.13} \ rm m _ {\ rm m _ {\ odot} $。 $ \ dot {p} _ {\ rm b} $的当前值与使用$ \dotΩ$和$ h_3 $获得的质量的GR期望一致。过量代表了该系统对偶极GWS发射的限制。这导致了$ |α_ {\ rm p}-α_ {\ rm c} |的脉冲星和伴侣的有效标量耦合差异限制（通过重力量理论； <4.8 \ times 10^{ - 3} $，不会为STT产生竞争性测试。但是，我们对该系统未来广告系列的模拟表明，到2032年，$ \ dot {p} _ {\ rm b} $和$ \dotΩ$的精确度将允许更加精确的群众，并且对偏面GWS的轨道衰减贡献更加严格，从而导致$ | rm |α_} {\ rm p。 C} | <1.3 \ times 10^{ - 3} $。我们还介绍了该系统将放置在2032年Def重力的$ \ {α_0，β_0\} $参数上。它们与PSR J1738+0333的参数相当。与PSR J1738+0333不同，PSR J1952+2630在其质量测量中不会受到限制，并且有可能在将来对DED重力更加限制。由于缺乏精确的距离测量值，这项测试的进一步改进可能会受到$ \ dot {p} _ {\ rm b} $的不确定性的限制。
We report the results of timing observations of PSR J1952+2630, a 20.7 ms pulsar in orbit with a massive white dwarf companion. With the increased timing baseline, we obtain improved estimates for astrometric, spin, and binary parameters for this system. We get an improvement of an order of magnitude on the proper motion, and, for the first time, we detect three post-Keplerian parameters in this system: the advance of periastron, the orbital decay, and the Shapiro delay. We constrain the pulsar mass to 1.20$^{+0.28}_{-0.29}\rm M_{\odot}$ and the mass of its companion to 0.97$^{+0.16}_{-0.13}\rm M_{\odot}$. The current value of $\dot{P}_{\rm b}$ is consistent with GR expectation for the masses obtained using $\dotω$ and $h_3$. The excess represents a limit on the emission of dipolar GWs from this system. This results in a limit on the difference in effective scalar couplings for the pulsar and companion (predicted by scalar-tensor theories of gravity; STTs) of $|α_{\rm p}-α_{\rm c}| < 4.8 \times 10^{-3}$, which does not yield a competitive test for STTs. However, our simulations of future campaigns of this system show that by 2032, the precision of $\dot{P}_{\rm b}$ and $\dotω$ will allow for much more precise masses and much tighter constraints on the orbital decay contribution from dipolar GWs, resulting in $|α_{\rm p}-α_{\rm c}|<1.3 \times 10^{-3}$. We also present the constraints this system will place on the $\{α_0,β_0\}$ parameters of DEF gravity by 2032. They are comparable to those of PSR J1738+0333. Unlike PSR J1738+0333, PSR J1952+2630 will not be limited in its mass measurement and has the potential to place even more restrictive limits on DEF gravity in the future. Further improvements to this test will likely be limited by uncertainties in the kinematic contributions to $\dot{P}_{\rm b}$ due to lack of precise distance measurements.
