TIDALLY INDUCED APSIDAL PRECESSION IN DOUBLE WHITE DWARFS: A NEW MASS MEASUREMENT TOOL WITH LISA
TIDALLY INDUCED APSIDAL PRECESSION IN DOUBLE WHITE DWARFS: A NEW MASS MEASUREMENT TOOL WITH LISA
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DOI：
10.1088/0004-637x/745/2/137
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发表时间：
2011-05
期刊：
影响因子：
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通讯作者：
F. Valsecchi;W. Farr;B. Willems;C. Deloye;V. Kalogera
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文献类型：
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作者：
F. Valsecchi;W. Farr;B. Willems;C. Deloye;V. Kalogera
银河系相互作用的双白色矮星（DWD）是激光干涉仪空间天线GW探测器的保证引力波（GW）源，预计在使命的生命周期内将探测到超过104个双星。这个人口的一部分，预计将是偏心的，在这里，我们调查的潜在约束白色矮（WD）的属性，通过拱点进动在这些双星。我们分析的潮汐，旋转，和广义相对论的贡献，拱点岁差通过使用详细的他WD模型，其中的星星的内部的演变是遵循整个冷却阶段。与以前的研究一致的零温度WD，我们发现，在偏心DWDs的拱点进动可以导致一个可检测到的转变时，发出的GW信号与冷（旧）组件被认为是二进制文件。对于热（年轻）WD，该偏移显著增加。我们发现，在热（冷）DWDs的拱点运动是占主导地位的潮汐在轨道频率高于10−4 Hz（10−3 Hz）。在这些源的拱点进动的分析，而忽略潮汐分量将导致一个极端的偏差，在质量的测定，并可能导致我们错误地识别WD作为中子星或黑洞。我们使用详细的WD模型表明，对于较老的，冷WD，有一个独特的关系，联系半径和拱点岁差常数WD群众，因此允许潮汐被用作一种工具来约束源群众。
Galactic interacting double white dwarfs (DWDs) are guaranteed gravitational wave (GW) sources for the Laser Interferometer Space Antenna GW detector, with more than 104 binaries expected to be detected over the mission's lifetime. Part of this population is expected to be eccentric, and here we investigate the potential for constraining the white dwarf (WD) properties through apsidal precession in these binaries. We analyze the tidal, rotational, and general relativistic contributions to apsidal precession by using detailed He WD models, where the evolution of the star's interior is followed throughout the cooling phase. In agreement with previous studies of zero-temperature WDs, we find that apsidal precession in eccentric DWDs can lead to a detectable shift in the emitted GW signal when binaries with cool (old) components are considered. This shift increases significantly for hot (young) WDs. We find that apsidal motion in hot (cool) DWDs is dominated by tides at orbital frequencies above ≳ 10−4 Hz (10−3 Hz). The analysis of apsidal precession in these sources while ignoring the tidal component would lead to an extreme bias in the mass determination, and could lead us to misidentify WDs as neutron stars or black holes. We use the detailed WD models to show that for older, cold WDs, there is a unique relationship that ties the radius and apsidal precession constant to the WD masses, therefore allowing tides to be used as a tool to constrain the source masses.