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Statistical Analysis of Individual Solar Active Regions

Published online by Cambridge University Press:  24 July 2018

Garyfallia Kromyda  and
Loukas Vlahos
Garyfallia Kromyda
Affiliation:
Department of Physics, Aristotle University of Thessaloniki GR-52124 Thessaloniki, Greece email: glkromyda@gmail.com
Loukas Vlahos
Affiliation:
Department of Physics, Aristotle University of Thessaloniki GR-52124 Thessaloniki, Greece email: vlahos@astro.auth.gr
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Abstract

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In the last decades, numerous observational and computational studies have shown that the global flare distribution is a power-law with a slope less than 2. In these studies, active regions are treated as statistically indistinguishable. To test this, we identify and separately analyze the flares produced by ten individual active regions (2006-2016). In five regions, we find a single power-law distribution, with a slope of a < 2. In the other five, we find a broken double power-law distribution, with slopes a1 < 2 and a2 > 2.

Keywords

Sun: coronaflaresX-raysradiation mechanisms: thermalmethods: statisticaldata analysis
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S335: Space Weather of the Heliosphere: Processes and Forecasts , July 2017 , pp. 3 - 6
Copyright
Copyright © International Astronomical Union 2018 

References

Aschwanden, M. et al. 2016, Space Science Reviews, 198, 47Google Scholar
Bak, P., Tang, C. & Wiesenfeld, K. 1987, Physical Review Letters vol. 59, p. 381-384CrossRefGoogle Scholar
Bak, P., Tang, C. & Wiesenfeld, K. 1988, Physical Review A, vol. 38, p. 364-374Google Scholar
Charbonneau, P. 2001, Solar Physics, 203, 321–353Google Scholar
Freeland, S. L. & Handy, B. N. 1998, Solar Physics, 182, Issue 2, 497-500Google Scholar
Georgoulis, M. & Vlahos, L. 1996, Astrophysical Journal, 496, L135CrossRefGoogle Scholar
Hudson, H. S. 1991, Solar Physics, 133, 357–369Google Scholar
Lu, E. T. & Hamilton, R. J. 1991, ApJ, 380, 89–92Google Scholar
Lu, E. T., Hamilton, R. J., McTiernan, J. M. & Bromund, K. R. 1993, ApJ, 412, 841–852Google Scholar
Parker, E. N. 1988, ApJ, 330, 474–479Google Scholar
Vlahos, L., Georgoulis, M., Kluiving, R. & Pascos, P. 1995, Astronomy and Astrophysics, 299, 897Google Scholar
Wheatland, M. S. 2010, ApJ, 710, 1324–1334Google Scholar