Improving Large-scale Convection Zone-to-Corona Models

Details Improving Large-scale Convection Zone-to-Corona Models Improving Large-scale Convection Zone-to-Corona Models

2010-05-04

arxiv.org/abs/1005.0641v1

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

9 pages, 4 figures. Mem. Soc. Astron. Ital., in press (2010)

Scientific paper

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.

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