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Monte Carlo radiative transfer for the nebular phase of Type Ia supernovae
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Number of Authors: 122020 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 492, no 2, p. 2029-2043Article in journal (Refereed) Published
Abstract [en]

We extend the range of validity of the ARTIS 3D radiative transfer code up to hundreds of days after explosion, when Type Ia supernovae (SNe Ia) are in their nebular phase. To achieve this, we add a non-local thermodynamic equilibrium population and ionization solver, a new multifrequency radiation field model, and a new atomic data set with forbidden transitions. We treat collisions with non-thermal leptons resulting from nuclear decays to account for their contribution to excitation, ionization, and heating. We validate our method with a variety of tests including comparing our synthetic nebular spectra for the well-known one-dimensional W7 model with the results of other studies. As an illustrative application of the code, we present synthetic nebular spectra for the detonation of a sub-Chandrasekhar white dwarf (WD) in which the possible effects of gravitational settling of Ne-22 prior to explosion have been explored. Specifically, we compare synthetic nebular spectra for a 1.06 M-circle dot WD model obtained when 5.5 Gyr of very efficient settling is assumed to a similar model without settling. We find that this degree of Ne-22 settling has only amodest effect on the resulting nebular spectra due to increased Ni-58 abundance. Due to the high ionization in sub-Chandrasekhar models, the nebular [Ni II] emission remains negligible, while the [Ni III] line strengths are increased and the overall ionization balance is slightly lowered in the model with Ne-22 settling. In common with previous studies of sub-Chandrasekhar models at nebular epochs, these models overproduce [Fe III] emission relative to [Fe II] in comparison to observations of normal SNe Ia.

Place, publisher, year, edition, pages
2020. Vol. 492, no 2, p. 2029-2043
Keywords [en]
atomic processes, line: formation, radiative transfer, methods: numerical, supernovae: general, white dwarfs
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:su:diva-179544DOI: 10.1093/mnras/stz3412ISI: 000512297600036OAI: oai:DiVA.org:su-179544DiVA, id: diva2:1412394
Available from: 2020-03-06 Created: 2020-03-06 Last updated: 2020-03-06Bibliographically approved

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Kromer, M.Bulla, Mattia
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Department of PhysicsThe Oskar Klein Centre for Cosmo Particle Physics (OKC)Nordic Institute for Theoretical Physics (Nordita)
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