Electronic Resource

The Black hole-neutron star binary merger in full general relativity : dependence on neutron star equations of state

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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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Ketersediaan

Informasi Detail

Judul Seri

Springer Theses

No. Panggil

E1795

Penerbit

Tokyo : Springer., 2013

Deskripsi Fisik

xiii, 178 hlm.

Bahasa

English

ISBN/ISSN

9784431542018

Klasifikasi

NONE

Tipe Isi

text

Tipe Media

computer

Tipe Pembawa

online resource

Edisi

-

Subjek

Astronomi
Fisika Numerik dan Komputasi
Astrofisika dan Kosmologi

Info Detail Spesifik

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Pernyataan Tanggungjawab

Koutarou Kyutoku

Versi lain/terkait

Lampiran Berkas

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