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The relationship between hard X-ray pulse timings and the locations of footpoint sources during solar flares View all abstracts by submitter

Andrew Inglis   Submitted: 2012-01-27 10:56

The cause of quasi-periodic pulsations (QPP) in solar flares remains the subject of debate. Recently, Nakariakov & Zimovets (2011) proposed a new model suggesting that, in two-ribbon flares, such pulsations could be explained by propagating slow waves. These waves may travel obliquely to the magnetic field, reflect in the chromosphere and constructively interfere at a spatially separate site in the corona, leading to quasi-periodic reconnection events progressing along the flaring arcade. Such a slow wave regime would have certain observational characteristics. We search for evidence of this phenomenon during a selection of two-ribbon flares observed by RHESSI, SOHO and TRACE; the flares of 2002 November 9, 2005 January 19 and 2005 August 22. We were not able to observe a clear correlation between hard X-ray footpoint separations and pulse timings during these events. Also, the motion of hard X-ray footpoints is shown to be continuous within the observational error, whereas a discontinuous motion might be anticipated in the slow wave model. Finally, we find that for a preferential slow wave propagation angle of 25-28 degrees that is expected for the fastest waves, the velocities of the hard X-ray footpoints lead to estimated pulse periods and ribbon lengths significantly larger than the measured values. Hence, for the three events studied, we conclude that the observational characteristics cannot be easily explained via the Nakariakov & Zimovets (2011) propagating slow wave model when only angles of 25-28 degrees are considered. We provide suggested flare parameters to optimise future studies of this kind.

Authors: A. R. Inglis & B. R. Dennis
Projects: RHESSI,SoHO-EIT,TRACE

Publication Status: ApJ (accepted)
Last Modified: 2012-01-27 22:34
Go to main E-Print page  Prominence seismology  Observations of Enhanced EUV Continua During An X-class Solar Flare Using SDO/EVE  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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