The solar flares of August 28 and 30, 1966
- Creators
- Zirin, Harold
- Lackner, D. Russo
Abstract
We describe observations of the class 3+ flare of August 28, 1966, made at the Mount Wilson Observatory. This great proton flare followed the sequence: (1) Precursor flare; (2) Filament eruption; (3) Beginning in penumbra of large spot; (4) Rapid elongation in two strands; (5) Great spray and surface wave; (6) Rapid separation of two strands to maximum brightness; and (7) Slow spread of brightness and decay. The soft X-ray burst coincides with stages 3–6, decaying through stage 7; the hard (> 80 keV) burst coincides, but decays more rapidly. Considering a demi-cylinder of emitting material, the soft X-rays are explained by a 4-million-degree plasma, or at least a large flux of electrons with that amount of energy. Given this flux, the microwave burst is explained by synchrotron emission with the low frequency cut-off due to coronal absorption. The class-2 flare of August 30, 1966, is also discussed.
Additional Information
© 1969 Kluwer Academic Publishers. Provided by the NASA Astrophysics Data System. Received 02 July 1968; Issue Date January 1969. This research was supported by the Advanced Research Projects Agency under the Office of Naval Research Grant N00014-67-C-0140 and the National Aeronautics and Space Administration under Grant NGR 05 002 034. NASA International University Fellow at the California Institute of Technology, 1967–1968, now at Arcetri Astrophysical Observatory.Attached Files
Published - 1969SoPh____6___86Z.pdf
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Additional details
- Eprint ID
- 104208
- Resolver ID
- CaltechAUTHORS:20200702-122854199
- Advanced Research Projects Agency (ARPA)
- N00014-67-C-0140
- Office of Naval Research (ONR)
- NGR 05 002 034
- NASA
- Created
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2020-07-02Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field