Dynamics of oscillating relativistic tori around Kerr black holes

被引:70
作者
Zanotti, O
Font, JA
Rezzolla, L
Montero, PJ
机构
[1] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain
[2] SISSA, Int Sch Adv Studies, I-34014 Trieste, Italy
[3] Ist Nazl Fis Nucl, I-34014 Trieste, Italy
[4] Louisiana State Univ, Dept Phys & Astron, Baton Rouge, LA 70803 USA
关键词
accretion; accretion discs; gravitational waves; hydrodynamics; relativity;
D O I
10.1111/j.1365-2966.2004.08567.x
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present a comprehensive numerical study of the dynamics of relativistic axisymmetric accretion tori with a power-law distribution of specific angular momentum orbiting in the background space-time of a Kerr black hole. By combining general relativistic hydrodynamics simulations with a linear perturbative approach we investigate the main dynamical properties of these objects over a large parameter space. The astrophysical implications of our results extend and improve two interesting results that have been recently reported in the literature. First, the induced quasi-periodic variation of the mass quadrupole moment makes relativistic tori of nuclear matter densities, as those formed during the last stages of binary neutron star mergers, promising sources of gravitational radiation, potentially detectable by interferometric instruments. Secondly, p-mode oscillations in relativistic tori of low rest-mass densities could be used to explain high-frequency quasi-periodic oscillations observed in X-ray binaries containing a black hole candidate under conditions more generic than those considered so far.
引用
收藏
页码:1371 / 1382
页数:12
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