The Value of Progenitor Radius Measurements for Explosion Modeling of Type II-Plateau Supernovae. (arXiv:2005.07290v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Goldberg_J/0/1/0/all/0/1">Jared A. Goldberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bildsten_L/0/1/0/all/0/1">Lars Bildsten</a>
Using Modules for Experiments in Stellar Astrophysics (MESA)+STELLA, we show
that very different physical models can adequately reproduce a specific
observed Type II-Plateau Supernova (SN). We consider SN2004A, SN2004et,
SN2009ib, SN2017eaw, and SN2017gmr, Nickel-rich ($M_mathrm{Ni}>0.03M_odot$)
events with bolometric lightcurves and a well-sampled decline from the plateau.
These events also have constraints on the progenitor radius, via a progenitor
image, or, in the case of SN2017gmr, a radius from fitting shock-cooling
models. In general, many explosions spanning the parameter space of progenitors
can yield excellent lightcurve and Fe line velocity agreement, demonstrating
the success of scaling laws in motivating models which match plateau properties
for a given radius and highlighting the degeneracy between plateau luminosity
and velocity in models and observed events, which can span over 50% in ejecta
mass, radius, and explosion energy. This can help explain disagreements in
explosion properties reported for the same event using different model
calculations. Our calculations yield explosion properties when combined with
pre-explosion progenitor radius measurements or a robust understanding of the
outermost $<0.1,M_odot$ of material that quantifies the progenitor radius
from SN observations a few days after explosion.
Using Modules for Experiments in Stellar Astrophysics (MESA)+STELLA, we show
that very different physical models can adequately reproduce a specific
observed Type II-Plateau Supernova (SN). We consider SN2004A, SN2004et,
SN2009ib, SN2017eaw, and SN2017gmr, Nickel-rich ($M_mathrm{Ni}>0.03M_odot$)
events with bolometric lightcurves and a well-sampled decline from the plateau.
These events also have constraints on the progenitor radius, via a progenitor
image, or, in the case of SN2017gmr, a radius from fitting shock-cooling
models. In general, many explosions spanning the parameter space of progenitors
can yield excellent lightcurve and Fe line velocity agreement, demonstrating
the success of scaling laws in motivating models which match plateau properties
for a given radius and highlighting the degeneracy between plateau luminosity
and velocity in models and observed events, which can span over 50% in ejecta
mass, radius, and explosion energy. This can help explain disagreements in
explosion properties reported for the same event using different model
calculations. Our calculations yield explosion properties when combined with
pre-explosion progenitor radius measurements or a robust understanding of the
outermost $<0.1,M_odot$ of material that quantifies the progenitor radius
from SN observations a few days after explosion.
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