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\section{Modeling the Supernova Shock-CSM Interaction to Infer Mass-loss History}  \begin{itemize}  \item  The variable radio emission from SN Ic encodes but does not directly yield the mass-loss history. To infer the mass-loss history, we must first model the radio emission from a supernova shock overtaking the CSM.\item  For relatively simple shock CSM interactions, Chavelier XXX and Chavelier XXX developed analytic solutions and set the language for shock-CSM interactions. However, it is very likely that the mass-loss history is more complicated and requires with multiple ejection events including some that are aspherical. Therefore, we will need to model the shock-CSM interations with  numerical simulations.\item  In principle, the shock-CSM  evolution is radiative and hydrodynamic. However, we will be considering the radio emission from 10 days until 1000 days. During much of this time, one may simply evolve the shock and CSM interaction hydrodynamically and post-process the radiation. In the spirit of building our knowledge, we will first consider spherically symmetric pre-explosion mass loss. simulations and explore.  There are plenty of examples of aspherical mass-loss, so we will also need to consider the signatures of aspherial ejection in the radio light curves.\item  But before we try to infer the aspherical character of the mass-loss from the radio lightcurves of SNe, we will first do forward modeling. We will take examples of observed aspherical ejections and model their radio light curves, exploring the systematics. It is unlikely that one can infer too many details about the asymmetry, so one goal is to characterize what broad aspherical characteristics one could infer.\item  To carry out these simulations, we will use Cufe, a hydro code. Cufe.  \end{itemize}