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Magneto-Acoustic Energetics Study of the Seismically Active Flare of 15 February 2011 View all abstracts by submitter

Julian David Alvarado-Gomez   Submitted: 2012-03-17 18:15

Multi-wavelength studies of energetic solar flares with seismic emissions have revealed interesting common features between them. We studied the first GOES X-class flare of the 24th solar cycle, as detected by the Solar Dynamics Observatory (SDO). For context, seismic activity from this flare (SOL2011-02-15T01:55-X2.2, in NOAA AR 11158) has been reported in the literature (Kosovichev, 2011; Zharkov et al., 2011). Based on Dopplergram data from the Helioseismic and Magnetic Imager (HMI), we applied standard methods of local helioseismology in order to identify the seismic sources in this event. RHESSI hard X-ray data are used to check the correlation between the location of the seismic sources and the particle precipitation sites in during the flare. Using HMI magnetogram data, the temporal profile of fluctuations in the photospheric line-of-sight magnetic field is used to estimate the magnetic field change in the region where the seismic signal was observed. This leads to an estimate of the work done by the Lorentz-force transient on the photosphere of the source region. In this instance this is found to be a significant fraction of the acoustic energy in the attendant seismic emission, suggesting that Lorentz forces can contribute significantly to the generation of sunquakes. However, there are regions in which the signature of the Lorentz-force is much stronger, but from which no significant acoustic emission emanates.

Authors: J.D. Alvarado-Gómez, J.C. Buitrago-Casas, J.C. Martínez-Oliveros, C. Lindsey, H. Hudson, B. Calvo-Mozo

Publication Status: Submitted to Solar Physics
Last Modified: 2012-03-19 14:13
Go to main E-Print page  Comparison of  Line-of-Sight Magnetograms Taken by the Solar Dynamics Observatory/Helioseismic and Magnetic Imager and  Solar and Heliospheric Observatory/Michelson Doppler Imager  Morphological evolution of a 3D CME cloud reconstructed from three viewpoints  Edit Entry  Download Preprint  Delete Entry 

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