Global MHD Models of the Solar Corona with Realistic Energy Transport*

Details Global MHD Models of the Solar Corona with Realistic Energy Transport* Global MHD Models of the Solar Corona with Realistic Energy Transport*

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsh52a..05l&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH52A-05

Physics

7509 Corona, 7524 Magnetic Fields, 7546 Transition Region, 7549 Ultraviolet Emissions, 2169 Solar Wind Sources

Scientific paper

Global MHD models of the corona and solar wind that use boundary conditions based on observed photospheric magnetic fields have now existed for more than a decade. Typically these models have avoided the complicated physics of the transition region by setting the ratio of specific heats (γ) to a reduced value. These "polytropic" MHD models have been successful in describing a number of aspects of coronal and heliospheric data, including the location of coronal holes, the reproduction of streamer structure as seen in white light, and the location of the heliospheric current sheet. The polytropic approach also has fundamental limitations, for example density and temperature contrasts between open and closed field regions do not match observations, and the model does not address data from EUV and X-ray emission. In this paper, we describe MHD models of the global corona that include energy transport (radiative losses, anisotropic thermal conduction, and coronal heating) in the transition region and solar corona and are capable of reproducing many emission properties as observed by SOHO and Yohkoh. These calculations are made tractable by a significant advance we have made in our ability to efficiently model the coupling between the transition region and corona. With this advance, it should be possible to routinely model the global corona, as is now possible with polytropic models. *Work supported by NASA, NSF and the Center for Integrated Space Weather Modeling (an NSF Science and Technology Center).

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