Global MHD Modeling of the Solar Corona and Inner Heliosphere for the Whole Heliosphere Interval

Details Global MHD Modeling of the Solar Corona and Inner Heliosphere for the Whole Heliosphere Interval Global MHD Modeling of the Solar Corona and Inner Heliosphere for the Whole Heliosphere Interval

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh53a..06r&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SH53A-06

Physics

7507 Chromosphere, 7509 Corona, 7511 Coronal Holes, 7524 Magnetic Fields, 7827 Kinetic And Mhd Theory

Scientific paper

Whole Heliosphere Interval (WHI), which runs from March 20 through April 16, 2008, and coincides with Carrington Rotation (CR) 2068 will provide a unique opportunity for both observers and modelers to collaborate in an effort to understand the three-dimensional structure and evolution of the solar corona and inner heliosphere. It builds on several previous "Whole Sun Month" intervals, which proved to be exceptionally successful. In support of WHI, we will develop a preliminary global MHD model solution for CR 2068. Our model, which includes energy transport processes, such as coronal heating, conduction of heat parallel to the magnetic field, radiative losses, and the effects of Alfven waves, is capable of producing significantly better estimates of the plasma temperature and density in the corona than have been possible in the past. With such a model, we can compute emission in extreme ultraviolet (EUV) and X-ray wavelengths, as well as scattering in polarized white light. Additionally, from our heliospheric solutions, we can deduce magnetic field and plasma parameters along specific spacecraft trajectories. Detailed comparisons of both remote solar and in situ observations with the model results will allow us to: (1) Connect these disparate set of observations; (2) Infer the global structure of the inner heliosphere; (3) Provide support for (or against) assumptions in the MHD model; and (4) Explore the effects of poorly understood physical processes, such as energy transport and/or differential rotation. We will make the results of these simulations (including post-processing analysis and visualization tools) available to the scientific community at iMHD.net/WHI.

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