Pulsations In Two-ribbon Flares: Waves, Reconnection Or Both?

Details Pulsations In Two-ribbon Flares: Waves, Reconnection Or Both? Pulsations In Two-ribbon Flares: Waves, Reconnection Or Both?

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.1204i&link_type=abstract

American Astronomical Society, SPD meeting #42, #12.04; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

Pulsations in flares, commonly observed simultaneously in hard X-rays and radio waves, are normally considered in the context of two alternate mechanisms: either a process of bursty reconnection, or a signature of periodic wave behaviour. However, observationally distinguishing between these mechanisms remains a challenging objective. By studying large two-ribbon flares with RHESSI, SOHO and now SDO, we attempt to discriminate between these two mechanisms by focusing on expected observable characteristics.
In particular, we focus on the recent slow wave model proposed by Nakariakov & Zimovets (2011). According to this model, slow waves propagate obliquely along the arcade, reflect from the chromosphere, and trigger reconnection in the corona due to constructive interference. Hence a discontinuous motion of footpoints along ribbons is expected, while the interval between pulses would be a function of footpoint separation. Additionally, gaps would be expected along the arcade in areas where magnetic reconnection was not triggered by waves and loops were not heated. The size of these gaps can be estimated from the preferential propagation angle of slow waves. We test for consistency with this model using observations of several flares, including from 9th November 2002 and 19th January 2005.
ARI is supported by the NASA Postdoctoral Programme, administered by Oak Ridge Associated Universities through a contract with NASA.

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