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Author
Korobkin, O.Wollaeger, R.T.
Fryer, C.L.
Hungerford, A.L.
Rosswog, S.
Fontes, C.J.
Mumpower, M.R.
Chase, E.A.
Even, W.P.
Miller, J.
Misch, G.W.
Lippuner, J.
Affiliation
University of ArizonaIssue Date
2021
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IOP Publishing LtdCitation
Korobkin, O., Wollaeger, R. T., Fryer, C. L., Hungerford, A. L., Rosswog, S., Fontes, C. J., ... & Lippuner, J. (2021). Axisymmetric Radiative Transfer Models of Kilonovae. The Astrophysical Journal, 910(2), 116.Journal
Astrophysical JournalRights
Copyright © 2021 The Author(s). Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
The detailed observations of GW170817 proved for the first time directly that neutron star mergers are a major production site of heavy elements. The observations could be fit by a number of simulations that qualitatively agree, but can quantitatively differ (e.g., in total r-process mass) by an order of magnitude. We categorize kilonova ejecta into several typical morphologies motivated by numerical simulations, and apply a radiative transfer Monte Carlo code to study how the geometric distribution of the ejecta shapes the emitted radiation. We find major impacts on both spectra and light curves. The peak bolometric luminosity can vary by two orders of magnitude and the timing of its peak by a factor of five. These findings provide the crucial implication that the ejecta masses inferred from observations around the peak brightness are uncertain by at least an order of magnitude. Mixed two-component models with lanthanide-rich ejecta are particularly sensitive to geometric distribution. A subset of mixed models shows very strong viewing angle dependence due to lanthanide "curtaining,"which persists even if the relative mass of lanthanide-rich component is small. The angular dependence is weak in the rest of our models, but different geometric combinations of the two components lead to a highly diverse set of light curves. We identify geometry-dependent P Cygni features in late spectra that directly map out strong lines in the simulated opacity of neodymium, which can help to constrain the ejecta geometry and to directly probe the r-process abundances. © 2021. The Author(s). Published by the American Astronomical Society.Note
Open access articleISSN
0004-637XVersion
Final published versionae974a485f413a2113503eed53cd6c53
10.3847/1538-4357/abe1b5
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Except where otherwise noted, this item's license is described as Copyright © 2021 The Author(s). Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.