Black hole-neutron star binary merger

Dependence on black hole spin orientation and equation of state

Kyohei Kawaguchi, Koutarou Kyutoku, Hiroyuki Nakano, Hirotada Okawa, Masaru Shibata, Keisuke Taniguchi

Research output: Contribution to journalArticle

45 Citations (Scopus)

Abstract

We systematically performed numerical-relativity simulations for black hole-neutron star (BH-NS) binary mergers with a variety of the BH spin orientation and nuclear-theory-based equations of state (EOS) of the NS. The initial misalignment angles of the BH spin measured from the direction of the orbital angular momentum are chosen in the range of itilt,0≈30°-90°. We employed four models of nuclear-theory-based zero-temperature EOS for the NS in which the compactness of the NS is in the range of C=MNS/RNS=0.138-0.180, where MNS and RNS are the mass and the radius of the NS, respectively. The mass ratio of the BH to the NS, Q=MBH/MNS, and the dimensionless spin parameter of the BH, χ, are chosen to be Q=5 and χ=0.75, together with MNS=1.35M so that the BH spin misalignment has a significant effect on tidal disruption of the NS. We obtain the following results: (i) The inclination angles of itilt,0<70° and itilt,0<50° are required for the formation of a remnant disk with its mass larger than 0.1M for the cases C=0.140 and C=0.160, respectively, while the disk mass is always smaller than 0.1M for C0.175. The ejecta with its mass larger than 0.01M is obtained for itilt,0<85° with C=0.140, for itilt,0<65° with C=0.160, and for itilt,0<30° with C=0.175. (ii) The rotational axis of the dense part of the remnant disk with its rest-mass density larger than 109g/cm3 is approximately aligned with the remnant BH spin for itilt,0≈30°. On the other hand, the disk axis is misaligned initially with ∼30° for itilt,0≈60°, and the alignment with the remnant BH spin is achieved at ∼50-60ms after the onset of merger. The accretion time scale of the remnant disk is typically ∼100ms and depends only weakly on the misalignment angle and the EOS. (iii) The ejecta velocity is typically ∼0.2-0.3c and depends only weakly on the misalignment angle and the EOS of the NS, while the morphology of the ejecta depends on its mass. (iv) The gravitational-wave spectra contains the information of the NS compactness in the cutoff frequency for itilt,0?60°.

Original languageEnglish
Article number024014
JournalPhysical Review D - Particles, Fields, Gravitation and Cosmology
Volume92
Issue number2
DOIs
Publication statusPublished - 2015 Jul 7

Fingerprint

neutron stars
equations of state
misalignment
ejecta
void ratio
mass ratios
gravitational waves
inclination
relativity
cut-off
angular momentum
alignment
orbitals
radii
simulation
temperature

ASJC Scopus subject areas

  • Nuclear and High Energy Physics

Cite this

Black hole-neutron star binary merger : Dependence on black hole spin orientation and equation of state. / Kawaguchi, Kyohei; Kyutoku, Koutarou; Nakano, Hiroyuki; Okawa, Hirotada; Shibata, Masaru; Taniguchi, Keisuke.

In: Physical Review D - Particles, Fields, Gravitation and Cosmology, Vol. 92, No. 2, 024014, 07.07.2015.

Research output: Contribution to journalArticle

Kawaguchi, Kyohei ; Kyutoku, Koutarou ; Nakano, Hiroyuki ; Okawa, Hirotada ; Shibata, Masaru ; Taniguchi, Keisuke. / Black hole-neutron star binary merger : Dependence on black hole spin orientation and equation of state. In: Physical Review D - Particles, Fields, Gravitation and Cosmology. 2015 ; Vol. 92, No. 2.
@article{c0724fac89314df59d7bb287235b97b0,
title = "Black hole-neutron star binary merger: Dependence on black hole spin orientation and equation of state",
abstract = "We systematically performed numerical-relativity simulations for black hole-neutron star (BH-NS) binary mergers with a variety of the BH spin orientation and nuclear-theory-based equations of state (EOS) of the NS. The initial misalignment angles of the BH spin measured from the direction of the orbital angular momentum are chosen in the range of itilt,0≈30°-90°. We employed four models of nuclear-theory-based zero-temperature EOS for the NS in which the compactness of the NS is in the range of C=MNS/RNS=0.138-0.180, where MNS and RNS are the mass and the radius of the NS, respectively. The mass ratio of the BH to the NS, Q=MBH/MNS, and the dimensionless spin parameter of the BH, χ, are chosen to be Q=5 and χ=0.75, together with MNS=1.35M so that the BH spin misalignment has a significant effect on tidal disruption of the NS. We obtain the following results: (i) The inclination angles of itilt,0<70° and itilt,0<50° are required for the formation of a remnant disk with its mass larger than 0.1M for the cases C=0.140 and C=0.160, respectively, while the disk mass is always smaller than 0.1M for C0.175. The ejecta with its mass larger than 0.01M is obtained for itilt,0<85° with C=0.140, for itilt,0<65° with C=0.160, and for itilt,0<30° with C=0.175. (ii) The rotational axis of the dense part of the remnant disk with its rest-mass density larger than 109g/cm3 is approximately aligned with the remnant BH spin for itilt,0≈30°. On the other hand, the disk axis is misaligned initially with ∼30° for itilt,0≈60°, and the alignment with the remnant BH spin is achieved at ∼50-60ms after the onset of merger. The accretion time scale of the remnant disk is typically ∼100ms and depends only weakly on the misalignment angle and the EOS. (iii) The ejecta velocity is typically ∼0.2-0.3c and depends only weakly on the misalignment angle and the EOS of the NS, while the morphology of the ejecta depends on its mass. (iv) The gravitational-wave spectra contains the information of the NS compactness in the cutoff frequency for itilt,0?60°.",
author = "Kyohei Kawaguchi and Koutarou Kyutoku and Hiroyuki Nakano and Hirotada Okawa and Masaru Shibata and Keisuke Taniguchi",
year = "2015",
month = "7",
day = "7",
doi = "10.1103/PhysRevD.92.024014",
language = "English",
volume = "92",
journal = "Physical review D: Particles and fields",
issn = "0556-2821",
publisher = "American Institute of Physics Publising LLC",
number = "2",

}

TY - JOUR

T1 - Black hole-neutron star binary merger

T2 - Dependence on black hole spin orientation and equation of state

AU - Kawaguchi, Kyohei

AU - Kyutoku, Koutarou

AU - Nakano, Hiroyuki

AU - Okawa, Hirotada

AU - Shibata, Masaru

AU - Taniguchi, Keisuke

PY - 2015/7/7

Y1 - 2015/7/7

N2 - We systematically performed numerical-relativity simulations for black hole-neutron star (BH-NS) binary mergers with a variety of the BH spin orientation and nuclear-theory-based equations of state (EOS) of the NS. The initial misalignment angles of the BH spin measured from the direction of the orbital angular momentum are chosen in the range of itilt,0≈30°-90°. We employed four models of nuclear-theory-based zero-temperature EOS for the NS in which the compactness of the NS is in the range of C=MNS/RNS=0.138-0.180, where MNS and RNS are the mass and the radius of the NS, respectively. The mass ratio of the BH to the NS, Q=MBH/MNS, and the dimensionless spin parameter of the BH, χ, are chosen to be Q=5 and χ=0.75, together with MNS=1.35M so that the BH spin misalignment has a significant effect on tidal disruption of the NS. We obtain the following results: (i) The inclination angles of itilt,0<70° and itilt,0<50° are required for the formation of a remnant disk with its mass larger than 0.1M for the cases C=0.140 and C=0.160, respectively, while the disk mass is always smaller than 0.1M for C0.175. The ejecta with its mass larger than 0.01M is obtained for itilt,0<85° with C=0.140, for itilt,0<65° with C=0.160, and for itilt,0<30° with C=0.175. (ii) The rotational axis of the dense part of the remnant disk with its rest-mass density larger than 109g/cm3 is approximately aligned with the remnant BH spin for itilt,0≈30°. On the other hand, the disk axis is misaligned initially with ∼30° for itilt,0≈60°, and the alignment with the remnant BH spin is achieved at ∼50-60ms after the onset of merger. The accretion time scale of the remnant disk is typically ∼100ms and depends only weakly on the misalignment angle and the EOS. (iii) The ejecta velocity is typically ∼0.2-0.3c and depends only weakly on the misalignment angle and the EOS of the NS, while the morphology of the ejecta depends on its mass. (iv) The gravitational-wave spectra contains the information of the NS compactness in the cutoff frequency for itilt,0?60°.

AB - We systematically performed numerical-relativity simulations for black hole-neutron star (BH-NS) binary mergers with a variety of the BH spin orientation and nuclear-theory-based equations of state (EOS) of the NS. The initial misalignment angles of the BH spin measured from the direction of the orbital angular momentum are chosen in the range of itilt,0≈30°-90°. We employed four models of nuclear-theory-based zero-temperature EOS for the NS in which the compactness of the NS is in the range of C=MNS/RNS=0.138-0.180, where MNS and RNS are the mass and the radius of the NS, respectively. The mass ratio of the BH to the NS, Q=MBH/MNS, and the dimensionless spin parameter of the BH, χ, are chosen to be Q=5 and χ=0.75, together with MNS=1.35M so that the BH spin misalignment has a significant effect on tidal disruption of the NS. We obtain the following results: (i) The inclination angles of itilt,0<70° and itilt,0<50° are required for the formation of a remnant disk with its mass larger than 0.1M for the cases C=0.140 and C=0.160, respectively, while the disk mass is always smaller than 0.1M for C0.175. The ejecta with its mass larger than 0.01M is obtained for itilt,0<85° with C=0.140, for itilt,0<65° with C=0.160, and for itilt,0<30° with C=0.175. (ii) The rotational axis of the dense part of the remnant disk with its rest-mass density larger than 109g/cm3 is approximately aligned with the remnant BH spin for itilt,0≈30°. On the other hand, the disk axis is misaligned initially with ∼30° for itilt,0≈60°, and the alignment with the remnant BH spin is achieved at ∼50-60ms after the onset of merger. The accretion time scale of the remnant disk is typically ∼100ms and depends only weakly on the misalignment angle and the EOS. (iii) The ejecta velocity is typically ∼0.2-0.3c and depends only weakly on the misalignment angle and the EOS of the NS, while the morphology of the ejecta depends on its mass. (iv) The gravitational-wave spectra contains the information of the NS compactness in the cutoff frequency for itilt,0?60°.

UR - http://www.scopus.com/inward/record.url?scp=84937122204&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84937122204&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.92.024014

DO - 10.1103/PhysRevD.92.024014

M3 - Article

VL - 92

JO - Physical review D: Particles and fields

JF - Physical review D: Particles and fields

SN - 0556-2821

IS - 2

M1 - 024014

ER -