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The Black Hole-Neutron Star Binary Merger in Full General Relativity - Dependence on Neutron Star Equations of State (Paperback, 2013 ed.)
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The Black Hole-Neutron Star Binary Merger in Full General Relativity - Dependence on Neutron Star Equations of State (Paperback, 2013 ed.)
Series: Springer Theses
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This thesis presents a systematic study of the orbital evolution,
gravitational wave radiation, and merger remnant of the black
hole-neutron star binary merger in full general relativity for the
first time. Numerical-relativity simulations are performed using an
adaptive mesh refinement code, SimulAtor for Compact objects in
Relativistic Astrophysics (SACRA), which adopts a wide variety of
zero-temperature equations of state for the neutron star matter.
Gravitational waves provide us with quantitative information on the
neutron star compactness and equation of state via the cutoff
frequency in the spectra, if tidal disruption of the neutron star
occurs before the binary merges. The cutoff frequency will be
observed by next-generation laser interferometric ground-based
gravitational wave detectors, such as Advanced LIGO, Advanced
VIRGO, and KAGRA. The author has also determined that the mass of
remnant disks are sufficient for the remnant black hole accretion
disk to become a progenitor of short-hard gamma ray bursts
accompanied by tidal disruptions and suggests that overspinning
black holes may not be formed after the merger of even an extremely
spinning black hole and an irrotational neutron star.
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