Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis
Abstract
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 ⊙ 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 ~10-6 M ⊙, 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 ~0.2 M ⊙ 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 thatmore »
- Authors:
-
- Institute for Advanced Study, Princeton, NJ (United States); Princeton Univ., NJ (United States). Dept. of Astrophysical Sciences
- Istituto Nazionale di Fisica Nucleare (INFN), Parma (Italy); Politecnico di Milano (Italy)
- Princeton Univ., NJ (United States). Dept. of Astrophysical Sciences
- Michigan State Univ., East Lansing, MI (United States). Dept. of Physics and Astronomy
- Istituto Nazionale di Fisica Nucleare (INFN), Parma (Italy); Friedrich Schiller Univ., Jena (Germany)
- Publication Date:
- Research Org.:
- Michigan State Univ., East Lansing, MI (United States); Krell Institute, Ames, IA (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC)
- OSTI Identifier:
- 1612794
- Grant/Contract Number:
- SC0017955; SC0019323
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal (Online)
- Additional Journal Information:
- Journal Name: The Astrophysical Journal (Online); Journal Volume: 869; Journal Issue: 2; Journal ID: ISSN 1538-4357
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 77 NANOSCIENCE AND NANOTECHNOLOGY; Astronomy & Astrophysics; nuclear reactions; nucleosynthesis; abundances; stars: neutron; Astrophysics - High Energy Astrophysical Phenomena
Citation Formats
Radice, David, Perego, Albino, Hotokezaka, Kenta, Fromm, Steven A., Bernuzzi, Sebastiano, and Roberts, Luke F. Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis. United States: N. p., 2018.
Web. doi:10.3847/1538-4357/aaf054.
Radice, David, Perego, Albino, Hotokezaka, Kenta, Fromm, Steven A., Bernuzzi, Sebastiano, & Roberts, Luke F. Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis. United States. https://doi.org/10.3847/1538-4357/aaf054
Radice, David, Perego, Albino, Hotokezaka, Kenta, Fromm, Steven A., Bernuzzi, Sebastiano, and Roberts, Luke F. Wed .
"Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis". United States. https://doi.org/10.3847/1538-4357/aaf054. https://www.osti.gov/servlets/purl/1612794.
@article{osti_1612794,
title = {Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis},
author = {Radice, David and Perego, Albino and Hotokezaka, Kenta and Fromm, Steven A. and Bernuzzi, Sebastiano and Roberts, Luke F.},
abstractNote = {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 ⊙ 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 ~10-6 M ⊙, 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 ~0.2 M ⊙ 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.},
doi = {10.3847/1538-4357/aaf054},
journal = {The Astrophysical Journal (Online)},
number = 2,
volume = 869,
place = {United States},
year = {Wed Dec 19 00:00:00 EST 2018},
month = {Wed Dec 19 00:00:00 EST 2018}
}
Web of Science
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