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.

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U2 - 10.1103/PhysRevD.87.024001

DO - 10.1103/PhysRevD.87.024001

M3 - Article

AN - SCOPUS:84871865650

VL - 87

JO - Physical Review D - Particles, Fields, Gravitation and Cosmology

JF - Physical Review D - Particles, Fields, Gravitation and Cosmology

SN - 1550-7998

IS - 2

M1 - 024001

ER -