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

295 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

ASJC Scopus subject areas

  • Nuclear and High Energy Physics
  • Physics and Astronomy (miscellaneous)

Fingerprint Dive into the research topics of 'Mass ejection from the merger of binary neutron stars'. Together they form a unique fingerprint.

  • 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