Modeling the Global Solar Corona with Improved Energy Transport

Details Modeling the Global Solar Corona with Improved Energy Transport Modeling the Global Solar Corona with Improved Energy Transport

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.1405m&link_type=abstract

American Astronomical Society, SPD meeting #37, #14.05; Bulletin of the American Astronomical Society, Vol. 38, p.244

Astronomy and Astrophysics

Astronomy

Scientific paper

We describe the application of a global three-dimensional magnetohydrodynamic (MHD) model of the solar corona that includes improved energy transport. The energy equation includes parameterized coronal heating, thermal conduction parallel to the magnetic field, radiative losses, and the acceleration due to Alfvén waves. This model makes it possible to determine the large-scale structure of the magnetic field in the corona, as well as the distribution of the solar wind velocity, plasma density, and temperature. The calculation uses the observed photospheric radial magnetic field as a boundary condition. We will describe the use of the model to predict the structure of the solar corona prior to the total solar eclipse that occurred on March 29, 2006. We used magnetic fields observed on the solar disk prior to eclipse day to predict what the corona will look like during the eclipse. The estimated coronal density and temperature was used to predict the plane-of-sky polarization brightness and emission of EUV and X-ray radiation. The prediction was posted on our web site (http://iMHD.net) prior to the eclipse. We will compare the prediction with eclipse observations..Supported by NASA's Sun-Earth Connection Theory and SR&T Programs and by NSF's CISM project

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