CORHEL MHD Modeling in Support of Solar Dynamics Observatory

Details CORHEL MHD Modeling in Support of Solar Dynamics Observatory CORHEL MHD Modeling in Support of Solar Dynamics Observatory

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21640217l&link_type=abstract

American Astronomical Society, AAS Meeting #216, #402.17; Bulletin of the American Astronomical Society, Vol. 41, p.876

Astronomy and Astrophysics

Astronomy

1

Scientific paper

CORHEL - for Corona-Heliosphere - is a coupled set of models and tools for quantitatively modeling the ambient solar corona and solar wind in various approximations. The coronal MHD code MAS in CORHEL has been used to produce routine polytropic solutions for all of the Carrington rotations during the STEREO mission (available at www.predsci.com). The MAS code can also be used to produce solutions that include energy transport (radiative losses, anisotropic thermal conduction, and coronal heating) in the transition region and solar corona. This more accurate representation of energy flow allows us to compute simulated EUV and X-ray emission and compare directly with observations. We refer to this as the thermodynamic MHD model. In this paper, we describe the production of thermodynamic MHD solutions as part of CORHEL. When sufficiently calibrated data are available, the solutions will use magnetic maps derived from HMI magnetograms. These solutions will be made routinely available in support of the Solar Dynamics Observatory (SDO) mission, and will allow comparison with emission observations from AIA when emission kernels become available.
Work supported by the LWS Strategic Capabilities Program (NASA, NSF, and AFOSR), CISM (NSF), HTP (NASA) and the HMI team.

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