X-rays, filament activity and flare prediction

Mosher, J. M.; Acton, L. W.

doi:10.1007/bf00150522

Cited by 4 publications

(1 citation statement)

References 12 publications

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“…In addition, the intensity variations before a fare are indistinguishable from the variations in the same active region when no flare occurs. For a more complete picture of the preflare-flare relationship these results should be combined with the fact that the flare does not typically occur at the site of the brightest preflare emission (Kahler, 1979) and that little or no correspondence exists between enhanced filament activity and soft X-ray brightening or likelihood for flaring (Mosher and Acton, 1980). The preflare heating phase included in the emerging flux model (Heyvaerts et al, 1977) and the unstable arch model (Spicer, 1977) of solar flares are not completely ruled out by these findings.…”

Section: Discussionmentioning

confidence: 99%

Soft X-ray emission from active regions shortly before solar flares

Wolfson¹

1982

Sol Phys

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Detailed examination of the variations in the intensity of soft X-ray emission prior to many solar flares are presented. In addition, these preflare intensity variations are contrasted with the variations typically observed for the same active regions in the absence of a flare. It is shown that a 5-20 min preflare brightening phase is not typically observed. These observations are discussed in context with other complimentary investigations and theoretical models.

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Section: Discussionmentioning

confidence: 99%

Soft X-ray emission from active regions shortly before solar flares

Wolfson¹

1982

Sol Phys

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Preflare Activity

Priest¹,

Gaizauskas²,

Hagyard³

et al. 1989

Energetic Phenomena on the Sun

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Preflare conditions, changes and events

Martin

1980

Sol Phys

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Preftare conditions, changes and events are loosely categorized as distinct, evolutionary or statistical. Distinct preflare phenomena are those for which direct physical associations with flares are implied. Also, they are not known to occur in a like manner during the absence of flares. These include the early stage of filament eruptions within active centers, preflare vortical structures, some transient X-ray emitting features, 5303 ~, accelerating coronal arches, and increases in circular polarization at cm wavelengths. Evolutionary preflare changes are considered to be any long-term effect that may be related to the flare build-up even though the same changes may occur in the absence of flares. This category covers the development of current sheets or strongly sheared magnetic fields, evolving magnetic features, emerging flux regions, the development of satellite fields around sunspots, the evolution of reverse polarity field configurations, the merging of adjacent active centers, sunspot motions and the development of velocity patterns. Statistical preflare changes logically include both distinct and evolutionary preflare changes. However, in addition, there are preflare conditions and events that are not necessarily linked to the flare in either a direct physical or indirect evolutionary way. Such parameters or events that may only be statistically significant are certain magnetic field properties, the brightness of active centers at various wavelengths, the previous occurrence of flares and subflares, increased turbulence in filaments and certain radio events.

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X-rays, filament activity and flare prediction

Cited by 4 publications

References 12 publications

Soft X-ray emission from active regions shortly before solar flares

Soft X-ray emission from active regions shortly before solar flares

Preflare Activity

Preflare conditions, changes and events

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