Filament eruptions and the impulsive phase of solar flares

Details Filament eruptions and the impulsive phase of solar flares Filament eruptions and the impulsive phase of solar flares

May 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...328..824k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 328, May 15, 1988, p. 824-829.

Astronomy and Astrophysics

Astrophysics

97

H Alpha Line, Plasma Heating, Solar Activity, Solar Corona, Solar Flares, Solar Prominences, Free Energy, Magnetohydrodynamic Stability, Particle Acceleration, Solar Atmosphere, Solar Magnetic Field

Scientific paper

Filament motion during the onset of the solar flare impulsive phase is examined. The impulsive phase onset is established from profiles of about 30 keV X-ray fluxes and the rapid flare brightenings characteristic of the H-alpha flash phase. The filament motion begins several minutes before the impulsive or flash phase of the flare. No new accleration is observed in the motion of the filament during the onset of the impulsive phase for at least two of the four flares. The most common H-alpha brightenings associated with the impulsive phase lie near the magnetic inversion line roughly centered under the erupting filament. Filament speeds at the onset of the impulsive or flash phase lie in the range 30-180 km/s. These characteristics indicate that the filament eruption is not driven by the flare plasma pressure, but instead marks an eruption of magnetic field driven by a global MHD instability of the field configuration in the region of the flare.

Affiliated with

Also associated with

No associations

Rating

Filament eruptions and the impulsive phase of solar flares does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Filament eruptions and the impulsive phase of solar flares, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Filament eruptions and the impulsive phase of solar flares will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-854115