Kavli Affiliate: Lars Bildsten
| First 5 Authors: Kathlynn Simotas, Kathlynn Simotas, , ,
| Summary:
Thermonuclear supernovae (SNe) are the result of the nuclear transformation
of carbon/oxygen (C/O) white dwarfs (WDs) to the radioactive element
$^56mathrmNi$ and intermediate mass elements (IMEs) like Ca, Ar, etc. Most
progenitor scenarios involve a companion star which donates matter to the
exploding white dwarf, implying a fundamental prediction: the formation of a
wake in the explosive ejecta as it runs into and moves past the companion star.
This wake leaves an indelible imprint on the ejecta’s density, velocity, and
composition structure that remains fixed as the ejecta reaches homologous
expansion. We simulate the interaction of the ejecta and Roche-lobe filling
donor in a double degenerate double detonation Type Ia progenitor scenario and
explore the detectability of this imprint in late-time nebular phase
spectroscopy of Type Ia SNe under the assumption of local heating ($t > 200$
days). At these times, the velocity profiles of forbidden emission lines
reflect the velocity distribution of all of the ejecta and the critical
electron density for that forbidden line. We explicitly calculate line shapes
for the [Co III] $11.89 mumathrmm$ line that traces the initial
$^56mathrmNi$ distribution and the [Ar III] $8.99 mumathrmm$ line,
which traces a typical intermediate mass element. We predict the viewing angle
dependence of the line shape, present a tool to quickly calculate optically
thin line shapes for various 3D density-velocity profiles and discuss JWST
observations.
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