scholarly journals General relativistic simulations of black-hole–neutron-star mergers: Effects of black-hole spin

2009 ◽  
Vol 79 (4) ◽  
Author(s):  
Zachariah B. Etienne ◽  
Yuk Tung Liu ◽  
Stuart L. Shapiro ◽  
Thomas W. Baumgarte
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Black Hole Spin ◽  
General Relativistic

scholarly journals Influence of the geometric configuration of accretion flow on the black hole spin dependence of relativistic acoustic geometry

2018 ◽  
Vol 27 (03) ◽  
pp. 1850023 ◽  
Author(s):  
Pratik Tarafdar ◽  
Tapas K. Das
Keyword(s):  
Black Hole ◽  
Kerr Black Hole ◽  
Geometric Configuration ◽  
Surface Gravity ◽  
Linear Perturbation ◽  
Flow Profile ◽  
White Hole ◽  
Accretion Flow ◽  
Black Hole Spin ◽  
General Relativistic

Linear perturbation of general relativistic accretion of low angular momentum hydrodynamic fluid onto a Kerr black hole leads to the formation of curved acoustic geometry embedded within the background flow. Characteristic features of such sonic geometry depend on the black hole spin. Such dependence can be probed by studying the correlation of the acoustic surface gravity [Formula: see text] with the Kerr parameter [Formula: see text]. The [Formula: see text]–[Formula: see text] relationship further gets influenced by the geometric configuration of the accretion flow structure. In this work, such influence has been studied for multitransonic shocked accretion where linear perturbation of general relativistic flow profile leads to the formation of two analogue black hole-type horizons formed at the sonic points and one analogue white hole-type horizon which is formed at the shock location producing divergent acoustic surface gravity. Dependence of the [Formula: see text]–[Formula: see text] relationship on the geometric configuration has also been studied for monotransonic accretion, over the entire span of the Kerr parameter including retrograde flow. For accreting astrophysical black holes, the present work thus investigates how the salient features of the embedded relativistic sonic geometry may be determined not only by the background spacetime, but also by the flow configuration of the embedding matter.

scholarly journals General relativistic simulations of black-hole–neutron-star mergers: Effects of magnetic fields

2012 ◽  
Vol 85 (6) ◽  
Author(s):  
Zachariah B. Etienne ◽  
Yuk Tung Liu ◽  
Vasileios Paschalidis ◽  
Stuart L. Shapiro
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Magnetic Fields ◽  
General Relativistic

scholarly journals Black hole-neutron star binary merger: Dependence on black hole spin orientation and equation of state

2015 ◽  
Vol 92 (2) ◽  
Author(s):  
Kyohei Kawaguchi ◽  
Koutarou Kyutoku ◽  
Hiroyuki Nakano ◽  
Hirotada Okawa ◽  
Masaru Shibata ◽  
...  
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Equation Of State ◽  
Spin Orientation ◽  
Black Hole Spin ◽  
Star Binary

scholarly journals Black hole-neutron star mergers: Effects of the orientation of the black hole spin

2011 ◽  
Vol 83 (2) ◽  
Author(s):  
Francois Foucart ◽  
Matthew D. Duez ◽  
Lawrence E. Kidder ◽  
Saul A. Teukolsky
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Black Hole Spin

scholarly journals Outflows from accretion discs formed in neutron star mergers: effect of black hole spin

2014 ◽  
Vol 446 (1) ◽  
pp. 750-758 ◽  
Author(s):  
Rodrigo Fernández ◽  
Daniel Kasen ◽  
Brian D. Metzger ◽  
Eliot Quataert
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Accretion Discs ◽  
Black Hole Spin

scholarly journals Coalescence of black hole–neutron star binaries

2021 ◽  
Vol 24 (1) ◽  
Author(s):  
Koutarou Kyutoku ◽  
Masaru Shibata ◽  
Keisuke Taniguchi
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Gravitational Wave ◽  
High Precision ◽  
Numerical Relativity ◽  
Current Status ◽  
Wave Spectra ◽  
Tidal Disruption ◽  
Merger Process ◽  
General Relativistic

AbstractWe review the current status of general relativistic studies for coalescences of black hole–neutron star binaries. First, high-precision computations of black hole–neutron star binaries in quasiequilibrium circular orbits are summarized, focusing on the quasiequilibrium sequences and the mass-shedding limit. Next, the current status of numerical-relativity simulations for the merger of black hole–neutron star binaries is described. We summarize our understanding for the merger process, tidal disruption and its criterion, properties of the merger remnant and ejected material, gravitational waveforms, and gravitational-wave spectra. We also discuss expected electromagnetic counterparts to black hole–neutron star coalescences.

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