Radiation Transport for Explosive Outflows: Opacity Regrouping

TL;DR

This paper advances radiation transport modeling in high-velocity outflows by developing a generalized opacity regrouping technique for IMC-DDMC, improving computational efficiency and enabling complex supernova simulations.

Contribution

It introduces a generalized non-contiguous opacity regrouping method for IMC-DDMC, enhancing speed and feasibility for supernova radiation transport modeling.

Findings

Opacity regrouping improves IMC-DDMC speed.

Regrouping is essential for feasible supernova simulations.

Good agreement between extit{supernu} and extit{phoenix} results.

Abstract

Implicit Monte Carlo (IMC) and Discrete Diffusion Monte Carlo (DDMC) are methods used to stochastically solve the radiative transport and diffusion equations, respectively. These methods combine into a hybrid transport-diffusion method we refer to as IMC-DDMC. We explore a multigroup IMC-DDMC scheme that, in DDMC, combines frequency groups with sufficient optical thickness. We term this procedure "opacity regrouping". Opacity regrouping has previously been applied to IMC-DDMC calculations for problems in which the dependence of the opacity on frequency is monotonic. We generalize opacity regrouping to non-contiguous groups and implement this in \supernu, a code designed to do radiation transport in high-velocity outflows with non-monotonic opacities. We find that regrouping of non-contiguous opacity groups generally improves the speed of IMC-DDMC radiation transport. We present an asymptotic analysis that informs the nature of the Doppler shift in DDMC groups and summarize the derivation of the Gentile-Fleck factor for modified IMC-DDMC. We test \supernu\ using numerical experiments including a quasi-manufactured analytic solution, a simple ten-group problem, and the W7 problem for Type Ia supernovae. We find that the opacity regrouping is necessary to make our IMC-DDMC implementation feasible for the W7 problem and possibly Type Ia supernova simulations in general. We compare the bolometric light curves and spectra produced by the \supernu\ and \phoenix\ radiation transport codes for the W7 problem. The overall shape of the bolometric light curves are in good agreement, as are the spectra and their evolution with time. However, for the numerical specifications we considered, we find that the peak luminosity of the light curve calculated using \supernu\ is $\sim$10% less than that calculated using \phoenix.