Shock Breakout in Dense Circumstellar Material with Application to PS1-13arp. (arXiv:2011.01937v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Haynie_A/0/1/0/all/0/1">Annastasia Haynie</a> (University of Southern California, Carnegie Observatories), <a href="http://arxiv.org/find/astro-ph/1/au:+Piro_A/0/1/0/all/0/1">Anthony L Piro</a> (Carnegie Observatories)
Shock breakout (SBO), the first expected electromagnetic signature of a
supernova (SN), can be an important probe of the progenitors of these
explosions. Unfortunately, SBO is difficult to capture with current surveys due
to its brief timescale ($lesssim 1,$hr). However, SBO may be lengthened when
dense circumstellar material (CSM) is present. Indeed, recent photometric
modeling studies of SNe, as well as early spectroscopy, suggest that such dense
CSM may be present more often than previously expected. If true, this should
also affect the features of SBO. We present an exploration of the impact of
such CSM interaction on the SBO width and luminosity using both analytic and
numerical modeling, where we parameterize the CSM as a steady-state wind. We
then compare this modeling to PS1-13arp, a SN that showed an early UV excess
that has been argued to be SBO in dense CSM. We find PS1-13arp is well fit with
a wind of mass $sim 0.08, M_{odot}$ and radius $sim 1900, R_{odot}$,
parameters which are similar to, if not slightly less massive than, what have
been inferred for Type II SNe using photometric modeling. This similarity
suggests that future SBO observations of SNe~II may be easier to obtain than
previously appreciated.
Shock breakout (SBO), the first expected electromagnetic signature of a
supernova (SN), can be an important probe of the progenitors of these
explosions. Unfortunately, SBO is difficult to capture with current surveys due
to its brief timescale ($lesssim 1,$hr). However, SBO may be lengthened when
dense circumstellar material (CSM) is present. Indeed, recent photometric
modeling studies of SNe, as well as early spectroscopy, suggest that such dense
CSM may be present more often than previously expected. If true, this should
also affect the features of SBO. We present an exploration of the impact of
such CSM interaction on the SBO width and luminosity using both analytic and
numerical modeling, where we parameterize the CSM as a steady-state wind. We
then compare this modeling to PS1-13arp, a SN that showed an early UV excess
that has been argued to be SBO in dense CSM. We find PS1-13arp is well fit with
a wind of mass $sim 0.08, M_{odot}$ and radius $sim 1900, R_{odot}$,
parameters which are similar to, if not slightly less massive than, what have
been inferred for Type II SNe using photometric modeling. This similarity
suggests that future SBO observations of SNe~II may be easier to obtain than
previously appreciated.
http://arxiv.org/icons/sfx.gif
