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From Solar Nanoflares to Stellar Giant Flares - Scaling Laws and Non-Implications for Coronal Heating View all abstracts by submitter

Markus J. Aschwanden   Submitted: 2006-12-04 14:41

In this study we explore physical scaling laws applied to solar nanoflares, microflares, and large flares, as well as to stellar giant flares. Solar flare phenomena exhibit a fractal volume scaling, V(L)lapprox L1.9, which explains the observed correlation EM_p propto T_p^4 between the total emission measure EM_p and flare peak temperature Tp in both solar and stellar flares. However, the detected stellar flares have higher emission measures EM_p than solar flares at the same flare peak temperature Tp, which can be explained by a higher electron density that is caused by shorter heating scale heights s_H/L approx 0.04-0.1 (with respect to the flare loop length L). Using these scaling laws we calculate the total radiated flare energies EX and thermal flare energies ET and find that the total counts C are a good proxy for both parameters. Comparing the energies of solar and stellar flares we find that even the smallest observed stellar flares exceed the largest solar flares, and thus their observed frequency distributions are hypothetically affected by an upper cutoff caused by the maximum active region size limit. The powerlaw slopes fitted near the upper cutoff can then not reliably be extrapolated to the microflare regime to evaluate their contribution to coronal heating.

Authors: Markus J. Aschwanden
Projects: TRACE

Publication Status: Advance in Space Science 39, 1867-1875 (2007), [Proc. COSPAR Meeting 2006, Beijing, China]
Last Modified: 2007-08-02 11:32
Go to main E-Print page  COMPUTING NONLINEAR FORCE-FREE CORONAL MAGNETIC FIELDS IN SPHERICAL GEOMETRY  Photospheric Magnetic Field Properties of Flaring Versus
Flare-Quiet Active Regions. IV. A Statistically Significant Sample  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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