Abstract
We have studied a series of flares in McMath 11482, 1972 August 19–22, with particular reference to the basis for the flares and comparison with dekameter radio data. We find that the flares were produced by rapid (∼ 1000 km h−1) westward motion of a large new p spot. Many flares occur just in front of the spot, and they cease when the motion stops. All flares occurring in front of the spot produce type III bursts, while even strong flares elsewhere in the region produce little or no type III. The time of type III emission agrees perfectly with the start of the Hα flare. Thus type III bursts are only produced in favorable configurations.
Simultaneous K-line movies are compared with Hα films and show little difference in flare appearance.
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References
Kane, S. and Donnelly, R. F.: 1971, Astrophys. J. 164, 151.
Ramaty, R. and Petrosian, V.: 1972, Astrophys. J. 178, 241.
Severny, A. B.: 1960, Izv. Krymsk. Astrofiz. Obs. 22, 12.
Zirin, H. and Werner, S.: 1967, Solar Phys. 1, 66.
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Zirin, H., Lazareff, B. Sunspot motion, flares and type III bursts in McMath 11482. Sol Phys 41, 425–438 (1975). https://doi.org/10.1007/BF00154079
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DOI: https://doi.org/10.1007/BF00154079