Major H alpha flares in centers of activity with very small or no spots
Helen W. Dodson,E. Ruth Hedeman +1 more
TLDR
In the years 1956-1968 these flares represented ∼ 7% of all confirmed flares of importance ⪖ 2 as mentioned in this paper, in which the flares were of unusually long duration and rose to maximum intensity slowly.Abstract:
Major Hα flares (importance ⪖ 2) in plages with only small or no spots constitute a rare but well observed aspect of solar activity. Information relating to 83 such flares has been assembled and studied. In the years 1956–1968 these flares represented ∼ 7% of all confirmed flares of importance ⪖ 2. In general, the flares were of unusually long duration and rose to maximum intensity slowly. A flash phase was often absent or poorly defined. In a number of cases, the flare emission included two bright filaments more or less parallel. The flares usually occurred during the late, flare-poor phase of a center of activity, and their outbreak did not presage a resurgence of activity in subsequent rotations. The flares were frequently associated with the position of dark filaments.read more
Citations
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Spotless flare activity
TL;DR: In this paper, the authors investigated the distribution of spotless flares (SFs) covering the time interval between 1947 and 1990 and found that the (11 − 20°) latitude zone was the most prolific region for the occurrence of SFs.
Journal ArticleDOI
A new and quantitative prediction scheme for solar flares
TL;DR: In this paper, a new and quantitative approach to predict the onset of the explosive process of solar flares and their intensity, based on the principle that solar flares are basically various manifestations of electromagnetic energy dissipation, so that a dynamo process in the photosphere as its power supply is essential.
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Statistical research into low-power solar flares. Main phase duration
TL;DR: In this paper, the authors used data from the International Flare Patrol, an electronic database of solar flares for the period 1972-2010 has been created, and they have identified more than 3000 cases with an ultra-long duration of the main phase (more than 60 minutes).
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Enhanced emission of Alfvén waves from sunspots during proton flares
TL;DR: In this paper, it is shown that in many proton flares, chromospheric emission overlies the umbra of a sunspot, indicating that the transition region between chromosphere and corona in the umbral flux tube has moved down to lower altitudes.
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Flares of spotless regions
TL;DR: In this article, an analysis of 20 flares of spotless regions observed at Yunnan Observatory during the peak years of Cycle 21 shows that the fraction of flares produced in these regions is about 3%, their Carrington longitudes show a tendency to drift eastward, and the majority of low energy flares are low-energy flares.
References
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Observation of a solar flare induced interplanetary shock and helium-enriched driver gas
TL;DR: In this paper, a solar flare induced interplanetary shock and helium enriched driver gas observed on 13 February 1967, discussing wind velocity and plasma acceleration were discussed. But the authors did not consider the effects of solar flares.
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Studies of solar protons with explorers xii and xiv
TL;DR: In this paper, four solar proton events observed by Explorers XII and XIV indicate that propagation of particles is a velocity dependent process, which is not the case for the current paper.
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A phenomenological model for disparitions brusques followed by flarelike chromospheric brightenings. i. the model, its consequences, and observations in quiet solar regions.
TL;DR: In this paper, a simple gravitational model for the flarelike brightenings of the chromosphere that follow most disparitions brusques (disappearing filaments) is presented, where the ascending prominence material is lifted out of the initially stable magnetic dips that characterize quiescent prominences and falls along the arched field lines into the bright areas.
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