deletions | additions       diff --git a/section_Modeling_the_Supernova_Shock__.tex b/section_Modeling_the_Supernova_Shock__.tex  index 49a14b8..cc66ed4 100644  --- a/section_Modeling_the_Supernova_Shock__.tex  +++ b/section_Modeling_the_Supernova_Shock__.tex 
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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 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. 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.   To carry out these simulations, we will use Cufe. Cufe (Murphy et al. 2015).