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Flaring Time Interval Distribution and Spatial Correlation of Major X-ray Flares View all abstracts by submitter

Yong-Jae Moon   Submitted: 2002-04-05 17:52

A statistical study is performed on X-ray flares stronger than C1 class that erupted during the solar maximum between 1989 and 1991. We have investigated the flaring time interval distribution (waiting-time distribution) and the spatial correlation of successive flare pairs. The observed waiting-time distribution for the whole data is found to be well represented by a nonstationary Poisson probability function with time varying mean flaring rates. The period most suitable for a constant mean flaring rate is determined to be 2-3 days by a Kolmogorov-Smirnov test. We have also found that the waiting-time distribution for flares in individual active regions follows a stationary Poisson probability function mexp(-mt) with a corresponding mean flaring rate. Therefore, the flaring probability within a given time is given by 1-exp(-mt), when the mean flaring rate m is properly estimated. It is also found that there is no systematic relationships between peak fluxes of flares and their waiting-time distributions. The above findings support the idea that the solar corona is in a self-organized critical state. A comparison of the angular distances of successively observed flare pairs with those of hypothetical flare pairs generated by random distribution shows a positive angular correlation within about 10 degrees (sim 180 arcsec in the observing field) of angular separation, which suggests that homologous flares occurring in the same active region should outnumber sympathetic flares.

Authors: Y.-J. Moon, G. S. Choe, H. S. Yun, Y. D. Park
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Publication Status: JGR-space physics, 2001, 106(A12), 29951-29961
Last Modified: 2002-04-05 17:52
Go to main E-Print page  OSCILLATING HOT LOOPS OBSERVED BY SUMER  Force-Freeness of Solar Magnetic  Fields in the Photosphere  Edit Entry  Download Preprint  Delete Entry 

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