000			03239nam a22004935i 4500
001			978-4-431-54201-8
003			DE-He213
005			20140220082926.0
007			cr nn 008mamaa
008			130125s2013 ja | s |||| 0|eng d
020			_a9784431542018 _9978-4-431-54201-8
024	7		_a10.1007/978-4-431-54201-8 _2doi
050		4	_aQB1-991
050		4	_aQB460-466
050		4	_aQB980-991
072		7	_aPGC _2bicssc
072		7	_aSCI004000 _2bisacsh
072		7	_aSCI005000 _2bisacsh
082	0	4	_a520 _223
100	1		_aKyutoku, Koutarou. _eauthor.
245	1	4	_aThe Black Hole-Neutron Star Binary Merger in Full General Relativity _h[electronic resource] : _bDependence on Neutron Star Equations of State / _cby Koutarou Kyutoku.
264		1	_aTokyo : _bSpringer Japan : _bImprint: Springer, _c2013.
300			_aXIII, 178 p. 46 illus. in color. _bonline resource.
336			_atext _btxt _2rdacontent
337			_acomputer _bc _2rdamedia
338			_aonline resource _bcr _2rdacarrier
347			_atext file _bPDF _2rda
490	1		_aSpringer Theses, Recognizing Outstanding Ph.D. Research, _x2190-5053
505	0		_aEquations of State of Neutron Star Matter -- Computing Initial Conditions -- Methods of Simulations -- Diagnostics for Numerical Simulations -- The Merger of Nonspinning Black Hole-Neutron Star Binaries -- The Merger of Spinning Black Hole-Neutron Star Binaries.
520			_aThis 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.
650		0	_aPhysics.
650		0	_aAstronomy.
650	1	4	_aPhysics.
650	2	4	_aAstronomy, Astrophysics and Cosmology.
650	2	4	_aMathematical Applications in the Physical Sciences.
650	2	4	_aNumerical and Computational Physics.
710	2		_aSpringerLink (Online service)
773	0		_tSpringer eBooks
776	0	8	_iPrinted edition: _z9784431542001
830		0	_aSpringer Theses, Recognizing Outstanding Ph.D. Research, _x2190-5053
856	4	0	_uhttp://dx.doi.org/10.1007/978-4-431-54201-8
912			_aZDB-2-PHA
999			_c99054 _d99054