Using X-ray and EUV Active Region Observations to Constrain the CoronalHeating Rate

Details Using X-ray and EUV Active Region Observations to Constrain the CoronalHeating Rate Using X-ray and EUV Active Region Observations to Constrain the CoronalHeating Rate

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.1702w&link_type=abstract

American Astronomical Society, SPD meeting #37, #17.02; Bulletin of the American Astronomical Society, Vol. 38, p.245

Astronomy and Astrophysics

Astronomy

Scientific paper

One constraint on the coronal heating mechanism may come from the observation that X-ray and EUV intensities of solar active regions are well correlated with the total unsigned magnetic flux. In this presentation, we discuss an extensive modeling effort using 26 active regions observed with EIT, SXT, and MDI. For each active region, we use potential field extrapolations of the photospheric field to estimate the coronal field. We then populate the resulting field lines with solutions to the hydrostatic loop equations assuming steady, uniform heating rates of the form E B^alpha/L^beta. We compare the resulting relationship between the simulated X-ray and EUV intensities and total unsigned flux with the observed relationship. We find that solutions with E B/L are the most consistent with the X-ray observations as well as the EUV "moss" intensities, but no heating function well matches the EUV loop intensities. Because static models are unable to address the extended emission at lower (1-2 MK) temperatures, we suggest that dynamical processes play a significant role in active region heating.

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