论文标题
V. Venkatraman Krishnan等人对二进制脉冲星系统中快速旋转的白色矮人引起的“透明式框架”的评论
A comment on "Lense-Thirring frame dragging induced by a fast-rotating white dwarf in a binary pulsar system" by V. Venkatraman Krishnan et al
论文作者
论文摘要
我们对最近的一项研究报告了一项研究证据，该证据是轨道平面的一般相对论晶状体的世俗进攻，直到轨道上的倾斜$ i $ i $ i $ to psr二进制系统的天空平面PSR J1141-6545由白色矮人和一个可比较质量的放射性放射线制成。二极管质量力矩$ q_2^\ mathrm {c} $和Angular动量$ {\ boldsymbol s}^\ Mathrm {c} $ of White dwarf导致脉搏脉冲时间对$ I $的可检测效果。 $ q_2^\ mathrm {c} $和$ {\ boldsymbol s}^\ mathrm {c} $在$ q_2^\ mathrm {c} $上做出的与历史有关的假设，即使只是为了计算结果后的预言，即可在依次进行测试中，即可依靠效果，甚至需要计算出来的分析表达式。此外，取决于如何计算$ q_2^\ mathrm {c} $，竞争性四极引起的变化速率（这是系统不确定性的主要来源）可能是$ \ yssim 30-50 \％\％\％\％的lense-thirring效果，大多数允许的值在3D参数spain fy the允许的效果中，由3D参数spand partic spand spains facepent a $ p_ \ mathrm {s} $，以及其旋转轴的极性角$ i_ \ mathrm {c}，\，ζ_\ mathrm {c} $。还研究了Periastron $ \ dot \ varpi $的经度的可能使用。事实证明，对其世俗进动的测量，除其他外，还由$ q_2^\ mathrm {c}，\，\，{\ boldsymbol {s}}}}^\ mathrm {c} $，可以帮助进一步限制White dwwarf param param param param paramemeter of White允许的区域。
We comment on a recent study reporting evidence for the general relativistic Lense-Thirring secular precession of the inclination $I$ of the orbital plane to the plane of the sky of the tight binary system PSR J1141-6545 made of a white dwarf and an emitting radiopulsar of comparable masses. The quadrupole mass moment $Q_2^\mathrm{c}$ and the angular momentum ${\boldsymbol S}^\mathrm{c}$ of the white dwarf cause the detectable effects on $I$ with respect to the present-day accuracy in the pulsar's timing. The history-dependent and model-dependent assumptions to be made on $Q_2^\mathrm{c}$ and ${\boldsymbol S}^\mathrm{c}$, required even just to calculate the analytical expressions for the resulting post-Keplerian precessions, may be deemed as too wide in order to claim a successful test of the Einsteinian gravitomagnetic effect. Moreover, depending on how $Q_2^\mathrm{c}$ is calculated, the competing quadrupole-induced rate of change, which is a major source of systematic uncertainty, may be up to $\lesssim 30-50\%$ of the Lense-Thirring effect for most of the allowed values in the 3D parameter space spanned by the white dwarf's spin period $P_\mathrm{s}$, and the polar angles $i_\mathrm{c},\,ζ_\mathrm{c}$ of its spin axis. The possible use of the longitude of periastron $\dot\varpi$ is investigated as well. It turns out that a measurement of its secular precession, caused, among other things, also by $Q_2^\mathrm{c},\,{\boldsymbol{S}}^\mathrm{c}$, could help in further restricting the permitted regions in the white dwarf's parameter space.
