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A statistical analysis of the soft X-ray profiles of solar flares

Published online by Cambridge University Press:  27 September 2017

G. Pearce  and
R.A. Harrison
G. Pearce
Affiliation:
Department of Astrophysics, Oxford University; , Jesus College, Oxford; , and Rutherford Appleton Laboratory
R.A. Harrison
Affiliation:
Astrophysics and Geophysics Division, Rutherford Appleton Laboratory

Extract

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We undertake a statistical analysis of the soft X-ray (3.5 – 5.5 keV) profiles of solar flares as observed with the Hard X-ray Imaging Spectrometer on the SMM. The durations, maximum intensities and intensity profiles of the flares are examined. The properties of the “typical” solar flare are discussed. The distributions of the measured parameters with respect to one another reveal some interesting results. In common with past studies, we conclude that there is no evidence to suggest that more than one type of event is being viewed, despite a desire evident in the literature to place events into distinct groups. We also conclude that commonly held views about the relatonships between flare duration and intensity, profile asymmetries and intensity etc.. are in error. For more details of the flare events, the selection of data and the method of analysis, the reader is referred to Pearce and Harrison (1988).

Type
Session II: Solar Flares
Information
International Astronomical Union Colloquium , Volume 104 , Issue 2: Solar and Stellar Flares , 1989 , pp. 161 - 164
Copyright
Copyright © Kluwer 1989

References

Culhane, J.L. and Phillips, K.J.H.; 1970, Solar Phys. 11, 117.CrossRefGoogle Scholar
Drake, J.F.: 1971, Solar Phys. 16, 152.Google Scholar
Pearce, G. and Harrison, R.A.: 1988, Astron. Astrophys. in press.Google Scholar
Phillips, K.J.H.: 1972, Ph.D. Thesis, University College London.Google Scholar