Improving Large-scale Convection Zone-to-Corona Models
Abstract
We introduce two new methods that are designed to improve the realism and utility of large, active region-scale 3D MHD models of the solar atmosphere. We apply these methods to RADMHD, a code capable of modeling the Sun's upper convection zone, photosphere, chromosphere, transition region, and corona within a single computational volume. We first present a way to approximate the physics of optically-thick radiative transfer without having to take the computationally expensive step of solving the radiative transfer equation in detail. We then briefly describe a rudimentary assimilative technique that allows a time series of vector magnetograms to be directly incorporated into the MHD system.
Cite
@article{arxiv.1005.0641,
title = {Improving Large-scale Convection Zone-to-Corona Models},
author = {William P. Abbett and George H. Fisher},
journal= {arXiv preprint arXiv:1005.0641},
year = {2010}
}
Comments
9 pages, 4 figures. Mem. Soc. Astron. Ital., in press (2010)