Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh32a..02m&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #SH32A-02
Astronomy and Astrophysics
Astrophysics
[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections
Scientific paper
We present progress on modeling Earth-directed CMEs including the December 12, 2008 CME and the May 13, 2005 campaign event from initiation to heliospheric propagation. Our earlier work on the 2005 event followed the CME to the orbit of Saturn employing the coronal model of Cohen et al. (2007), which relies on a spatially varying adiabatic index (gamma) to produce the bimodal solar wind. This model was able to reproduce several features of the observed event, but suffered from artifacts of the artificially thermodynamics. We will examine results of a recent simulation performed with a new two-temperature solar corona model developed at the University of Michigan. This model employs heat conduction for both ion and electron species, constant adiabatic index (=5/3), and includes Alfven waves to drive the solar wind. The model includes SOHO/MDI magnetogram data to calculate the coronal field, and also uses SOHO/EIT observations to specify the density and temperature at the coronal boundary by the Differential Emission Measure Tomography (DEMT) method. The Wang-Sheeley-Arge empirical model is used to determine the Alfven wave pressure necessary to produce the observed solar wind speeds. We find that the new model is much better able to reproduce the solar wind densities, and also correctly captures the compression at the CME-driven shock due to the fixed adiabatic index.
der Holst Bart van
Frazin Richard A.
Gombosi Tamas I.
Manchester Ward B.
Tóth Géza
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