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

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh21c..02r&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH21C-02

Physics

2102 Corotating Streams, 2134 Interplanetary Magnetic Fields, 2164 Solar Wind Plasma, 2169 Solar Wind Sources, 7511 Coronal Holes

Scientific paper

Whole Heliosphere Interval (WHI), which runs from March 20 through April 16, 2008, and coincides with Carrington Rotation (CR) 2068 is providing 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 have developed a 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. In this presentation, we make detailed comparisons of both remote solar and in situ observations with the model results. Such comparisons allow us and (3) Provide support for (or against) assumptions in the MHD model, such as which physical processes are (or are not) important. The results of these simulations (including post-processing analysis and visualization tools) will be made available to the scientific community at http://predsci.com/WHI.

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