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On the relationship between soft X-rays and H-alpha-emitting structures during a solar flareBased on data obtained during a solar flare on March 31, 1979, soft X-ray (SXR) and hard X-ray (HXR) bursts are analyzed and compared with other available data in order to identify structures in H-alpha that may correspond to the SXR-emitting site. Measurements taken with the X-ray telescope and the XUV spectroheliograph flown on Skylab, have shown that the SXR emission from many flares comes from rather small structures of about 10-20 arcsec across. These structures appear to be loops that cross the magnetic neutral line. Understanding of the morphology of SXR was based on data of the solar flare of June 15, 1973, observed from Skylab, and the work of Moore et al., (1980). Dense, highly emissive coronal structures, not suggested to be the X-ray source, were forming, lost energy rapidly by emission and conduction, and finally formed the loops. It is concluded that bright H-alpha loops form rapidly as the SXR emission rises, and the overall decay (cooling rate) of SXR emission is much slower than the formation time of individual loops.
Document ID
19810050853
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Zirin, H.
(Big Bear Solar Observatory Pasadena, Calif., United States)
Feldman, U.
(Hale Observatories Pasadena, CA, United States)
Doschek, G. A.
(U.S. Navy, Naval Research Laboratory, Washington D.C., United States)
Kane, S.
(California, University Berkeley, Calif., United States)
Date Acquired
August 11, 2013
Publication Date
May 15, 1981
Publication Information
Publication: Astrophysical Journal
Subject Category
Solar Physics
Accession Number
81A35257
Funding Number(s)
CONTRACT_GRANT: NGL-05-002-034
CONTRACT_GRANT: NSF ATM-79-11139
Distribution Limits
Public
Copyright
Other

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