期刊
ASTROPHYSICAL JOURNAL
卷 869, 期 2, 页码 -出版社
IOP Publishing Ltd
DOI: 10.3847/1538-4357/aaf054
关键词
nuclear reactions, nucleosynthesis, abundances; stars: neutron
资金
- Frank and Peggy Taplin Membership at the Institute for Advanced Study
- Max-Planck/Princeton Center (MPPC) for Plasma Physics [NSF PHY-1523261]
- INFN initiative High Performance data Network - CIPE
- Institute for Nuclear Theory
- Institute for Advanced Study
- United States Department of Energy through the Computational Science Graduate Fellowship [DE-SC0019323]
- EU H2020 under ERC Starting grant [BinGraSp-714626]
- US Department of Energy [DE-SC0017955]
- NSF PRAC program [ACI-1440083, AWD-1811236]
- NSF XSEDE program [TG-PHY160025]
- Princeton Institute for Computational Science and Engineering (PICSciE)
- Princeton University Office of Information Technology
- Michigan State University
- U.S. Department of Energy (DOE) [DE-SC0017955] Funding Source: U.S. Department of Energy (DOE)
We present a systematic numerical relativity study of the mass ejection and the associated electromagnetic transients and nucleosynthesis from binary neutron star (NS) mergers. We find that a few 10(-3)M(circle dot) of material is ejected dynamically during the mergers. The amount and the properties of these outflows depend on binary parameters and on the NS equation of state (EOS). A small fraction of these ejecta, typically similar to 10(-6)M(circle dot), is accelerated by shocks formed shortly after merger to velocities larger than 0.6c and produces bright radio flares on timescales of weeks, months, or years after merger. Their observation could constrain the strength with which the NSs bounce after merger and, consequently, the EOS of matter at extreme densities. The dynamical ejecta robustly produce second and third r-process peak nuclei with relative isotopic abundances close to solar. The production of light r-process elements is instead sensitive to the binary mass ratio and the neutrino radiation treatment. Accretion disks of up to similar to 0.2M(circle dot) are formed after merger, depending on the lifetime of the remnant. In most cases, neutrino- and viscously driven winds from these disks dominate the overall outflow. Finally, we generate synthetic kilonova light curves and find that kilonovae depend on the merger outcome and could be used to constrain the NS EOS.
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