Black hole tidal problem in the Fermi normal coordinates
Black hole tidal problem in the Fermi normal coordinates
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DOI：
10.1103/physrevd.71.044017
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发表时间：
2005-01
影响因子：
5
通讯作者：
Masaki Ishii;M. Shibata;Y. Mino
中科院分区：
文献类型：
--
作者：
Masaki Ishii;M. Shibata;Y. Mino
本文导出了自引力流体星星绕克尔黑洞沿着类时测地线运动时的潮汐势，推广了Fishbone和Marck以前的工作。本文在Manasse和Misner提出的框架下，在Fermi正规坐标系中计算了三阶和四阶R/r项的潮汐位，其中R为恒星半径，r为轨道间距。新的公式被应用于确定的潮汐扰动极限（罗氏极限）的共转牛顿星的圆形轨道上运动的克尔黑洞的赤道平面。结果表明，对于R/r >或近似R/r的近轨道，三阶项和四阶项在Roche极限中起着重要的定量作用。0.1.研究还表明，中子星在最内层稳定圆轨道附近绕恒星质量黑洞运行时的洛希极限可能敏感地依赖于中子星星的状态方程。
We derive a tidal potential for a self-gravitating fluid star orbiting a Kerr black hole along a timelike geodesic, extending previous works by Fishbone and Marck. In this paper, the tidal potential is calculated up to the third- and fourth-order terms in R/r, where R is the stellar radius and r the orbital separation, in the Fermi normal coordinate system following the framework developed by Manasse and Misner. The new formulation is applied for determining the tidal disruption limit (Roche limit) of corotating Newtonian stars in circular orbits moving on the equatorial plane of Kerr black holes. It is demonstrated that the third- and fourth-order terms quantitatively play an important role in the Roche limit for close orbits with R/r > or approx. 0.1. It is also indicated that the Roche limit of neutron stars orbiting a stellar-mass black hole near the innermost stable circular orbit may depend sensitively on the equation of state of the neutron star.