3D Radiative Transfer with PHOENIX

TL;DR

This paper presents the development of the PHOENIX code for 3D radiative transfer, incorporating moving flows with a novel affine method, advancing the modeling of stellar atmospheres and supernovae spectra.

Contribution

The paper introduces a generalized 3D radiative transfer method in PHOENIX that accurately handles moving flows using a new affine approach, extending previous 1D solutions.

Findings

Successful implementation of 3D radiative transfer in PHOENIX

Exact treatment of moving flows with the affine method

Application to supernovae spectroscopy

Abstract

Using the methods of general relativity Lindquist derived the radiative transfer equation that is correct to all orders in v/c. Mihalas developed a method of solution for the important case of monotonic velocity fields with spherically symmetry. We have developed the generalized atmosphere code PHOENIX, which in 1-D has used the framework of Mihalas to solve the radiative transfer equation (RTE) in 1-D moving flows. We describe our recent work including 3-D radiation transfer in PHOENIX and particularly including moving flows exactly using a novel affine method. We briefly discuss quantitative spectroscopy in supernovae.