Heating Distribution Along Coronal Loops in two Active Regions Using a Simple Electrodynamic Calculation

Details Heating Distribution Along Coronal Loops in two Active Regions Using a Simple Electrodynamic Calculation Heating Distribution Along Coronal Loops in two Active Regions Using a Simple Electrodynamic Calculation

Jul 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aspc..424...25g&link_type=abstract

Proceedings of the 9th International Conference of the Hellenic Astronomical Society, proceedings of a conference held 20-24 Sep

Astronomy and Astrophysics

Astronomy

Scientific paper

The heating along hundreds of coronal loops of non flaring active regions is computed using a simple electrodynamic model. Photospheric motions generate electric fields inducing, electric potential differences at the footpoints of loops. These potential differences generate electric currents that lead to Ohmic heating. We computed the magnetic field extrapolation from the magnetograms of two active regions, namely NOAA AR 9366 (SOHO/MDI) and NOAA AR 10963, (HINODE/SOT). Closed magnetic field lines model the coronal loops. For each loop we computed the heating function and obtained the hydrostatic distribution of temperature and pressure. We found that the coronal heating is stronger near the footpoints of the loops and asymmetric along them. We obtained scaling laws that correlate the mean volumetric heating with the loop length, and the heating flux, through the loop footpoints with the magnetic field strength at the footpoints. Our results are in qualitative agreement with observations (see Gontikakis et al. 2008 for more details).

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