Titlebook: Coronal Disturbances; Gordon Newkirk Book 1974 International Astronomical Union 1974 Corona.Planet.Solar flare.Variation.cosmic ray.observ

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Total Quality Management — worldwide effectpassively, in virtually all coronal disturbances. The purpose of this paper is to put into perspective the various roles magnetic fields can play in both exciting and guiding these observed transient phenomena. A discussion of our present theoretical concepts relevant to this subject can be convenie

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TQM Structure and top-down requirementsr which the magnetic synoptic charts are available) the largest solar activity, usually connected with proton-flare occurrence, has been very closely related to a characteristic large-scale pattern in the magnetic field distribution with a life-time of the order of 8–10 solar rotations. These regula

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needle

II–VI electroluminescent deviceson on the NE limb (Gabriel ., 1971). The condensation shows the existence of loop structure, which defines the local magnetic fields, and is apparent in forbidden lines including those of Si ., Si ., S ., Fe ., Fe . and Fe . which lie between 1200 Å and 2050 Å (Jordan, 1971). These lines are formed

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II–VI electroluminescent devicesacteristics of the impulsive (flash) phase phenomenon in small solar flares particularly from the point of view of the acceleration of electrons and their role in producing the various impulsive phase emissions. Observed and deduced characteristics of the various electromagnetic emission sources are

chance

Bulk growth of widegap II–VI single crystalsory (Figure 1) provide a basis for correlation studies (especially timing information) of the associated white light flare, the high energy particle emission, type II bursts, and many other phenomena. This is perhaps the first time that sufficient radio coverage (i.e., data above 10000 MHz) was avai

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Bulk growth of widegap II–VI single crystals5694 have been used. Most of the observed phenomena are flare-connected, but all of them are related to some kind of Hα-activity. Sudden brightening of the emission lines may occur after the disappearance of a filament. The events have a duration of up to several hours and consist of hot clouds of h

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