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Title:
Study of the Seismically Active Flare of July 16, 2004
Authors:
Besliu-Ionescu, D.; Donea, A. C.; Cally, P.; Lindsey, C.
Affiliation:
AA(Centre for Stellar and Planetary Astrophysics, School of Mathematical Sciences, Monash University, Victoria 3800, Australia; Astronomical Institute of the Romanian Academy, RO-040557 Bucharest, Romania), AB(Centre for Stellar and Planetary Astrophysics, School of Mathematical Sciences, Monash University, Victoria 3800, Australia), AC(Centre for Stellar and Planetary Astrophysics, School of Mathematical Sciences, Monash University, Victoria 3800, Australia), AD(Colorado Research Associates Division, NorthWest Research Associates Inc., 3380 Mitchell Lane, Boulder, CO 80301, USA)
Publication:
Romanian Astronomical Journal Vol. 17 (2007), Supplement, p. 83-89
Publication Date:
00/2007
Origin:
AUTHOR
Keywords:
solar flares, sunquakes, H&alpha, observations
Bibliographic Code:
2007RoAJ...17S..83B

Abstract

Sunquakes have proven to be the most powerful events occurring at the solar surface. They are triggered by the impulsive flares produced in the corona, just above the acoustically active regions. Not every impulsive flare produces seismic waves emanating from the highly depressed photosphere, just beneath the flare. So far, we have identified a few mechanisms which can deliver acoustic energy into the photosphere: 1) the back-warming radiation suddenly heating the photosphere; 2) a strong shock-like compression wave propagating downwards into the chromosphere; 3) relativistic particles delivering directly the energy and momentum into the photosphere; and, 4) probably the magnetic tension at the feet of the loops. In order to discriminate which of these is the most efficient or dominated during a particular acoustically active flare, we have analysed the coronal and chromospheric emission of the regions just above the seismic source. We have performed a multiwavelength analysis of the active region 10649 that hosted the acoustically active solar flare of July 16, 2004. The spatial coincidence between the emissions at different layers of the sun, from the photosphere to the corona, suggests that high-energy particles travel through the coronal layers from the reconnection site, hit the solar chromosphere warming it up, which then, responds by sending further into the photosphere enough energy (carried either by the shock wave or by the Balmer and Pachen radiation) to produce a seismic event.
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