Semi-Empirically Derived Heating Function of the Corona-Heliopshere During the Whole- Sun Month

Details Semi-Empirically Derived Heating Function of the Corona-Heliopshere During the Whole- Sun Month Semi-Empirically Derived Heating Function of the Corona-Heliopshere During the Whole- Sun Month

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh23b0354g&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH23B-0354

Physics

7509 Corona, 7511 Coronal Holes, 7524 Magnetic Fields, 7599 General Or Miscellaneous

Scientific paper

In spite of many recent developments in observations and models of the solar corona, the exact form of the heating function of the solar wind plasma is unknown. Here we attempt to make some progress on that problem by applying a previously developed simplified magnetohydrodynamic model to a unique synthesis of remote sensing coronal observations from SOHO and Spartan 201 and in-situ data from Ulysses during the quiescent phase of solar cycle 23 (1995-1997) which also included the Whole Sun Month (August/September, 1996) study period. Our analysis provides for the first time an empirically derived estimate of the heat flux and temperature profile of the corona and interplanetary medium as a function of latitude and radial distance for this data set. Our results suggest that the effective heat flux and temperature may include thermal and non-thermal components possibly providing as much as half of the total heat input. The primary contribution of our analysis is that parameters calculated from our model provide insight into the energy deposition profile and the model results can be used as a test of observations of flow speed and temperature using different observational techniques for this period. The main limitations of the model are calculations of the magnetic field in equatorial regions, and the neglect of force balance across field lines.

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