Dynamics, nucleosynthesis, and kilonova signature of black hole—neutron star merger ejecta
Abstract
Here we investigate the ejecta from black hole—neutron star mergers by modeling the formation and interaction of mass ejected in a tidal tail and a disk wind. The outflows are neutron-rich, giving rise to optical/infrared emission powered by the radioactive decay of r-process elements (a kilonova). Here we perform an end-to-end study of this phenomenon, where we start from the output of a fully-relativistic merger simulation, calculate the post-merger hydrodynamical evolution of the ejecta and disk winds including neutrino physics, determine the final nucleosynthetic yields using post-processing nuclear reaction network calculations, and compute the kilonova emission with a radiative transfer code. We study the effects of the tail-to-disk mass ratio by scaling the tail density. A larger initial tail mass results in fallback matter becoming mixed into the disk and ejected in the subsequent disk wind. Relative to the case of a disk without dynamical ejecta, the combined outflow has lower mean electron fraction, faster speed, larger total mass, and larger absolute mass free of high-opacity Lanthanides or Actinides. In most cases, the nucleosynthetic yield is dominated by the heavy r-process contribution from the unbound part of the dynamical ejecta. A Solar-like abundance distribution can however be obtained when themore »
- Authors:
-
- University of Alberta, Edmonton, AB (Canada); University of California, Berkeley, CA (United States)
- Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States). Nuclear Science Division
- University of California, Berkeley, CA (United States); Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States). Nuclear Science Division
- California Institute of Technology (CalTech), Pasadena, CA (United States)
- University of California, Berkeley, CA (United States)
- Michigan State University, East Lansing, MI (United States)
- Publication Date:
- Research Org.:
- Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), Nuclear Physics (NP); National Science Foundation (NSF); National Aeronautics and Space Administration (NASA); University of Alberta; USDOE National Nuclear Security Administration (NNSA)
- OSTI Identifier:
- 1523373
- Grant/Contract Number:
- AC02-05CH11231; AST-1206097; PF4-150122; NAS8-03060
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Classical and Quantum Gravity
- Additional Journal Information:
- Journal Volume: 34; Journal Issue: 15; Journal ID: ISSN 0264-9381
- Publisher:
- IOP Publishing
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; accretion; accretion disks; dense matter; gravitational waves; hydrodynamics; neutrinos; nuclear reactions; nucleosynthesis; abundances.
Citation Formats
Fernández, Rodrigo, Foucart, Francois, Kasen, Daniel, Lippuner, Jonas, Desai, Dhruv, and Roberts, Luke F. Dynamics, nucleosynthesis, and kilonova signature of black hole—neutron star merger ejecta. United States: N. p., 2017.
Web. doi:10.1088/1361-6382/aa7a77.
Fernández, Rodrigo, Foucart, Francois, Kasen, Daniel, Lippuner, Jonas, Desai, Dhruv, & Roberts, Luke F. Dynamics, nucleosynthesis, and kilonova signature of black hole—neutron star merger ejecta. United States. https://doi.org/10.1088/1361-6382/aa7a77
Fernández, Rodrigo, Foucart, Francois, Kasen, Daniel, Lippuner, Jonas, Desai, Dhruv, and Roberts, Luke F. Tue .
"Dynamics, nucleosynthesis, and kilonova signature of black hole—neutron star merger ejecta". United States. https://doi.org/10.1088/1361-6382/aa7a77. https://www.osti.gov/servlets/purl/1523373.
@article{osti_1523373,
title = {Dynamics, nucleosynthesis, and kilonova signature of black hole—neutron star merger ejecta},
author = {Fernández, Rodrigo and Foucart, Francois and Kasen, Daniel and Lippuner, Jonas and Desai, Dhruv and Roberts, Luke F.},
abstractNote = {Here we investigate the ejecta from black hole—neutron star mergers by modeling the formation and interaction of mass ejected in a tidal tail and a disk wind. The outflows are neutron-rich, giving rise to optical/infrared emission powered by the radioactive decay of r-process elements (a kilonova). Here we perform an end-to-end study of this phenomenon, where we start from the output of a fully-relativistic merger simulation, calculate the post-merger hydrodynamical evolution of the ejecta and disk winds including neutrino physics, determine the final nucleosynthetic yields using post-processing nuclear reaction network calculations, and compute the kilonova emission with a radiative transfer code. We study the effects of the tail-to-disk mass ratio by scaling the tail density. A larger initial tail mass results in fallback matter becoming mixed into the disk and ejected in the subsequent disk wind. Relative to the case of a disk without dynamical ejecta, the combined outflow has lower mean electron fraction, faster speed, larger total mass, and larger absolute mass free of high-opacity Lanthanides or Actinides. In most cases, the nucleosynthetic yield is dominated by the heavy r-process contribution from the unbound part of the dynamical ejecta. A Solar-like abundance distribution can however be obtained when the total mass of the dynamical ejecta is comparable to the mass of the disk outflows. The kilonova has a characteristic duration of 1 week and a luminosity of ~ 1041 erg s-1 , with orientation effects leading to variations of a factor ~2 in brightness. At early times (< 1 d) the emission includes an optical component from the (hot) Lanthanide-rich material, but the spectrum evolves quickly to the infrared thereafter.},
doi = {10.1088/1361-6382/aa7a77},
journal = {Classical and Quantum Gravity},
number = 15,
volume = 34,
place = {United States},
year = {Tue Jul 04 00:00:00 EDT 2017},
month = {Tue Jul 04 00:00:00 EDT 2017}
}
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