Magnetic Storms by Roger Dean

By Roger Dean

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Published by way of the yank Geophysical Union as a part of the Geophysical Monograph Series.

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101, 13,943, 1996. 33 Priest, E. R. ), Solar Flare Magnetohydrodynamics, Gordon and Breach, N e w York, 1981. Priest, E. R. ), Dynamics and Structure of Quiescent Solar Prominences, Kluwer, Dordrecht, 1989. Riddle, A. , 13, 4 4 8 , 1970. Robinson, R. , Flare continuum, in Solar Radiophysics, edited by D. J. McLean and N . R. Labrum, chapter 15, Cambridge Univ. Press, Cambridge, 1985. D. thesis, University of Tokyo, 1994. T. Kosugi, S. M a s u d a etal, H a r d X-ray imaging observations by Yohkoh of the 1991 November 15 solar flare, Publ.

The en­ ergy may be comparable to that of the largest flare. As CMEs are an erupting phenomenon expanding outwards from the upper corona into interplanetary space, it is not surprising if they are statistically more geoeffective than flares; in fact geomagnetic storms 32 7 1 1 32 16 are known to be better associated with CMEs (especially those with larger velocities and masses) than flares [Gosling et ai, 1991]. Then, how are CMEs related to flares and what causes CMEs to erupt? A CME cannot be the simple aftermath of a flare explosion for several reasons.

Astr. Soc. Japan, 44, L63, 1992a. , T. Takahashi, L. W. Acton etal, Observation of a solar flare at the limb with the Yohkoh Soft X-ray Telescope, Publ. Astr. Soc. Japan, 44, L211, 1992b. Tsurutani, B. T. and W. D. Gonzalez, The interplanetary causes of magnetic storms: a review, in these proceed­ ings. Uchida, Y. and K. , 116, 291, 1988. , A. McAllister, K. T. Strong et al, Continual expansion of the active-region corona observed by the Yohkoh soft X-ray telescope, Publ. Astr. Soc. Japan, 44, L155, 1992.

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