Mass ejection from the merger of binary neutron stars

Kenta Hotokezaka, Kenta Kiuchi, Koutarou Kyutoku, Hirotada Okawa, Yu Ichiro Sekiguchi, Masaru Shibata, Keisuke Taniguchi

Research output: Contribution to journalArticle

244 Citations (Scopus)

Abstract

Numerical-relativity simulations for the merger of binary neutron stars are performed for a variety of equations of state (EOSs) and for a plausible range of the neutron-star mass, focusing primarily on the properties of the material ejected from the system. We find that a fraction of the material is ejected as a mildly relativistic and mildly anisotropic outflow with the typical and maximum velocities ∼0.15-0.25c and ∼0.5-0.8c (where c is the speed of light), respectively, and that the total ejected rest mass is in a wide range 10 -4-10-2M⊙, which depends strongly on the EOS, the total mass, and the mass ratio. The total kinetic energy ejected is also in a wide range between 1049 and 1051 ergs. The numerical results suggest that for a binary of canonical total mass 2.7M ⊙, the outflow could generate an electromagnetic signal observable by the planned telescopes through the production of heavy-element unstable nuclei via the r-process or through the formation of blast waves during the interaction with the interstellar matter, if the EOS and mass of the binary are favorable ones.

Original languageEnglish
Article number024001
JournalPhysical Review D - Particles, Fields, Gravitation and Cosmology
Volume87
Issue number2
DOIs
Publication statusPublished - 2013 Jan 2
Externally publishedYes

Fingerprint

binary stars
ejection
neutron stars
equations of state
interstellar matter
heavy elements
blasts
mass ratios
relativity
kinetic energy
telescopes
electromagnetism
nuclei
simulation
interactions

ASJC Scopus subject areas

  • Nuclear and High Energy Physics

Cite this

Hotokezaka, K., Kiuchi, K., Kyutoku, K., Okawa, H., Sekiguchi, Y. I., Shibata, M., & Taniguchi, K. (2013). Mass ejection from the merger of binary neutron stars. Physical Review D - Particles, Fields, Gravitation and Cosmology, 87(2), [024001]. https://doi.org/10.1103/PhysRevD.87.024001

Mass ejection from the merger of binary neutron stars. / Hotokezaka, Kenta; Kiuchi, Kenta; Kyutoku, Koutarou; Okawa, Hirotada; Sekiguchi, Yu Ichiro; Shibata, Masaru; Taniguchi, Keisuke.

In: Physical Review D - Particles, Fields, Gravitation and Cosmology, Vol. 87, No. 2, 024001, 02.01.2013.

Research output: Contribution to journalArticle

Hotokezaka, K, Kiuchi, K, Kyutoku, K, Okawa, H, Sekiguchi, YI, Shibata, M & Taniguchi, K 2013, 'Mass ejection from the merger of binary neutron stars', Physical Review D - Particles, Fields, Gravitation and Cosmology, vol. 87, no. 2, 024001. https://doi.org/10.1103/PhysRevD.87.024001
Hotokezaka, Kenta ; Kiuchi, Kenta ; Kyutoku, Koutarou ; Okawa, Hirotada ; Sekiguchi, Yu Ichiro ; Shibata, Masaru ; Taniguchi, Keisuke. / Mass ejection from the merger of binary neutron stars. In: Physical Review D - Particles, Fields, Gravitation and Cosmology. 2013 ; Vol. 87, No. 2.
@article{35c7822c161941278884dbb9f2a8c22f,
title = "Mass ejection from the merger of binary neutron stars",
abstract = "Numerical-relativity simulations for the merger of binary neutron stars are performed for a variety of equations of state (EOSs) and for a plausible range of the neutron-star mass, focusing primarily on the properties of the material ejected from the system. We find that a fraction of the material is ejected as a mildly relativistic and mildly anisotropic outflow with the typical and maximum velocities ∼0.15-0.25c and ∼0.5-0.8c (where c is the speed of light), respectively, and that the total ejected rest mass is in a wide range 10 -4-10-2M{\^a}Š™, which depends strongly on the EOS, the total mass, and the mass ratio. The total kinetic energy ejected is also in a wide range between 1049 and 1051 ergs. The numerical results suggest that for a binary of canonical total mass 2.7M {\^a}Š™, the outflow could generate an electromagnetic signal observable by the planned telescopes through the production of heavy-element unstable nuclei via the r-process or through the formation of blast waves during the interaction with the interstellar matter, if the EOS and mass of the binary are favorable ones.",
author = "Kenta Hotokezaka and Kenta Kiuchi and Koutarou Kyutoku and Hirotada Okawa and Sekiguchi, {Yu Ichiro} and Masaru Shibata and Keisuke Taniguchi",
year = "2013",
month = "1",
day = "2",
doi = "10.1103/PhysRevD.87.024001",
language = "English",
volume = "87",
journal = "Physical review D: Particles and fields",
issn = "0556-2821",
publisher = "American Institute of Physics Publising LLC",
number = "2",

}

TY - JOUR

T1 - Mass ejection from the merger of binary neutron stars

AU - Hotokezaka, Kenta

AU - Kiuchi, Kenta

AU - Kyutoku, Koutarou

AU - Okawa, Hirotada

AU - Sekiguchi, Yu Ichiro

AU - Shibata, Masaru

AU - Taniguchi, Keisuke

PY - 2013/1/2

Y1 - 2013/1/2

N2 - Numerical-relativity simulations for the merger of binary neutron stars are performed for a variety of equations of state (EOSs) and for a plausible range of the neutron-star mass, focusing primarily on the properties of the material ejected from the system. We find that a fraction of the material is ejected as a mildly relativistic and mildly anisotropic outflow with the typical and maximum velocities ∼0.15-0.25c and ∼0.5-0.8c (where c is the speed of light), respectively, and that the total ejected rest mass is in a wide range 10 -4-10-2M⊙, which depends strongly on the EOS, the total mass, and the mass ratio. The total kinetic energy ejected is also in a wide range between 1049 and 1051 ergs. The numerical results suggest that for a binary of canonical total mass 2.7M ⊙, the outflow could generate an electromagnetic signal observable by the planned telescopes through the production of heavy-element unstable nuclei via the r-process or through the formation of blast waves during the interaction with the interstellar matter, if the EOS and mass of the binary are favorable ones.

AB - Numerical-relativity simulations for the merger of binary neutron stars are performed for a variety of equations of state (EOSs) and for a plausible range of the neutron-star mass, focusing primarily on the properties of the material ejected from the system. We find that a fraction of the material is ejected as a mildly relativistic and mildly anisotropic outflow with the typical and maximum velocities ∼0.15-0.25c and ∼0.5-0.8c (where c is the speed of light), respectively, and that the total ejected rest mass is in a wide range 10 -4-10-2M⊙, which depends strongly on the EOS, the total mass, and the mass ratio. The total kinetic energy ejected is also in a wide range between 1049 and 1051 ergs. The numerical results suggest that for a binary of canonical total mass 2.7M ⊙, the outflow could generate an electromagnetic signal observable by the planned telescopes through the production of heavy-element unstable nuclei via the r-process or through the formation of blast waves during the interaction with the interstellar matter, if the EOS and mass of the binary are favorable ones.

UR - http://www.scopus.com/inward/record.url?scp=84871865650&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84871865650&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.87.024001

DO - 10.1103/PhysRevD.87.024001

M3 - Article

VL - 87

JO - Physical review D: Particles and fields

JF - Physical review D: Particles and fields

SN - 0556-2821

IS - 2

M1 - 024001

ER -