期刊
CLASSICAL AND QUANTUM GRAVITY
卷 34, 期 15, 页码 -出版社
IOP Publishing Ltd
DOI: 10.1088/1361-6382/aa7a77
关键词
accretion; accretion disks; dense matter; gravitational waves; hydrodynamics; neutrinos; nuclear reactions; nucleosynthesis; abundances
类别
资金
- University of California Office of the President
- NSF [AST-1206097]
- Faculty of Science at the University of Alberta
- NASA - Chandra x-ray Center [PF4-150122]
- Smithsonian Astrophysical Observatory for NASA [NAS8-03060]
- Department of Energy Office of Nuclear Physics Early Career Award
- Office of Energy Research, Office of High Energy and Nuclear Physics, Divisions of Nuclear Physics, of the US Department of Energy [DE-AC02-05CH11231]
- Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]
- Office of the CIO
- Direct For Mathematical & Physical Scien
- Division Of Physics [1565546] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Physics [1430152] Funding Source: National Science Foundation
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 similar to 10(41) erg s(-1), with orientation effects leading to variations of a factor similar to 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.
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