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Scaling Laws for Solar and Stellar Flares View all abstracts by submitter

Markus J. Aschwanden   Submitted: 2006-12-19 16:34

In this study we compile for the first time comprehensive data sets of solar and stellar flare parameters, including flare peak temperatures Tp, flare peak volume emission measures EM_p, and flare durations au_f from both solar and stellar data, as well as flare length scales L from solar data. Key results are that both the solar and stellar data are consistent with a common scaling law of EM_p propto T_p^4, but the stellar data exhibit a approx 250 times higher emission measure (at the same flare peak temperature). We apply the classical RTV scaling law and the generalized Serio scaling law to both the solar and stellar data. The major findings are: (1) The flare volume has a (non-Euclidian) fractal scaling of V(L) propto LD_V with D_V=2.0pm0.1, (2) Serio's scaling law can reproduce both the solar and stellar datasets, yielding significantly higher electron densities and smaller flare volumina than the classical RTV law, (3) both solar and stellar flares require footpoint-concentrated heating with a heating scale height ratio of 0.04 lapprox s_H/L lapprox 0.1 for stars and 0.1 lapprox s_H/L lapprox 1.0 for the Sun, (4) the detected solar flares have flare loop half lengths of 10 lapprox L lapprox 50 Mm, and (5) the electron densities in stellar flares are significantly larger (n_e approx 1012-1014 cm-3) than in solar flares (n_e approx 109-1012 cm-3). The obtained results allow us also to infer realistic radiative and conductive cooling times, thermal energies, and frequency distributions of solar and stellar flare energies.

Authors: Markus J. Aschwanden, Robert A. Stern, & Manuel Guedel
Projects: TRACE

Publication Status: ApJ (subm) - Dec 2006
Last Modified: 2006-12-20 11:35
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