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Dynamical mass ejection from the merger of asymmetric binary neutron stars: Radiation-hydrodynamics study in general relativity

Yuichiro Sekiguchi1, Kenta Kiuchi2, Koutarou Kyutoku3, Masaru Shibata2, and Keisuke Taniguchi4

  • 1Department of Physics, Toho University, Funabashi, Chiba 274-8510, Japan
  • 2Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan
  • 3Interdisciplinary Theoretical Science (iTHES) Research Group, RIKEN, Wako, Saitama 351-0198, Japan
  • 4Department of Physics, University of the Ryukyus, Nishihara, Okinawa 903-0213, Japan

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Phys. Rev. D 93, 124046 – Published 17 June, 2016

DOI: https://doi.org/10.1103/PhysRevD.93.124046

Abstract

We perform neutrino radiation-hydrodynamics simulations for the merger of asymmetric binary neutron stars in numerical relativity. Neutron stars are modeled by soft and moderately stiff finite-temperature equations of state (EOS). We find that the properties of the dynamical ejecta such as the total mass, neutron richness profile, and specific entropy profile depend on the mass ratio of the binary systems for a given EOS in a unique manner. For a soft EOS (SFHo), the total ejecta mass depends weakly on the mass ratio, but the average of electron number per baryon (Ye) and specific entropy (s) of the ejecta decreases significantly with the increase of the degree of mass asymmetry. For a stiff EOS (DD2), with the increase of the mass asymmetry degree, the total ejecta mass significantly increases while the average of Ye and s moderately decreases. We find again that only for the SFHo, the total ejecta mass exceeds 0.01M⊙ irrespective of the mass ratio chosen in this paper. The ejecta have a variety of electron number per baryon with an average approximately between Ye∼0.2 and ∼0.3 irrespective of the EOS employed, which is well suited for the production of the rapid neutron capture process heavy elements (second and third peaks), although its averaged value decreases with the increase of the degree of mass asymmetry.

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Phys. Rev. D 93, 124046– Published 17 June, 2016
  • Received 6 March 2016

© 2016 American Physical Society

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