### 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_{âŠ™}, 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 _{âŠ™}, 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 language | English |
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Article number | 024001 |

Journal | Physical Review D - Particles, Fields, Gravitation and Cosmology |

Volume | 87 |

Issue number | 2 |

DOIs | |

Publication status | Published - 2013 Jan 2 |

Externally published | Yes |

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### ASJC Scopus subject areas

- Nuclear and High Energy Physics

### Cite this

*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.

Research output: Contribution to journal › Article

*Physical Review D - Particles, Fields, Gravitation and Cosmology*, vol. 87, no. 2, 024001. https://doi.org/10.1103/PhysRevD.87.024001

}

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 -4-10-2MâŠ™, 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 âŠ™, 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 -4-10-2MâŠ™, 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 âŠ™, 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 -