Emission line models for the lowest-mass core collapse supernovae. I:
Case study of a 9 M_ one-dimensional neutrino-driven explosion
release_4mippsx74vh33dzby4w6zzv6be
by
A. Jerkstrand, T. Ertl, H.-T. Janka, E. Müller, T. Sukhbold, S. E.
Woosley
2017
Abstract
A large fraction of core-collapse supernovae (CCSNe), 30-50
originate from the low-mass end of progenitors with M_ ZAMS =
8-12 M_. However, degeneracy effects make stellar evolution modelling of
such stars challenging, and few predictions for their supernova light curves
and spectra have been presented. Here we calculate synthetic nebular spectra of
a 9 M_ Fe CCSN model exploded with the neutrino mechanism. The model
predicts emission lines with FWHM∼1000 km/s, including signatures from
each deep layer in the metal core. We compare this model to observations of the
three subluminous IIP SNe with published nebular spectra; SN 1997D, SN 2005cs,
and SN 2008bk. The prediction of both line profiles and luminosities are in
good agreement with SN 1997D and SN 2008bk. The close fit of a model with no
tuning parameters provides strong evidence for an association of these objects
with low-mass Fe CCSNe. For SN 2005cs, the interpretation is less clear, as the
observational coverage ended before key diagnostic lines from the core had
emerged. We perform a parameterised study of the amount of explosively made
stable nickel, and find that none of these three SNe show the high
^58Ni/^56Ni ratio predicted by current models of electron capture SNe
(ECSNe) and ECSN-like explosions. Combined with clear detection of lines from O
and He shell material, these SNe rather originate from Fe core progenitors. We
argue that the outcome of self-consistent explosion simulations of low-mass
stars, which gives fits to many key observables, strongly suggests that the
class of subluminous Type IIP SNe is the observational counterpart of the
lowest mass CCSNe.
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