Study of Ribbon Separation and Magnetic Reconnection Rates in a Two-Ribbon Flare

Details Study of Ribbon Separation and Magnetic Reconnection Rates in a Two-Ribbon Flare Study of Ribbon Separation and Magnetic Reconnection Rates in a Two-Ribbon Flare

Feb 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009soph..254..271x&link_type=abstract

Solar Physics, Volume 254, Issue 2, pp.271-283

Physics

4

Solar Activity, Solar Flares, Solar Magnetic Fields

Scientific paper

In this paper, we present a study of the correlation between the speed of flare ribbon separation and the magnetic flux density during the 10 April 2001 solar flare. The study includes the section of the neutral line containing the flare core and its peripheral area. This event shows clear two-ribbon structure and inhomogeneous magnetic fields along the ribbons, so the spatial correlation and distribution of the flare and magnetic parameters can be studied. A weak negative correlation is found between the ribbon separation speed ( V r) and the longitudinal magnetic flux density ( B z ). This correlation is the weakest around the peak of the flare. Spatially, the correlation is also weakest at the positions of the hard X-ray (HXR) sources. In addition, we estimate the magnetic reconnection rate (electric field strength in the reconnection region E rec) by combining the speed of flare ribbons and the longitudinal magnetic flux density. During flare evolution, the time profiles of the magnetic reconnection rate are similar to that of the ribbon separation speed, and the speeds of ribbon separation are relatively slow in the strong magnetic fields ( i.e., V r is negatively correlated with B z ). However, along the flare ribbons, E rec fluctuates in a small range except near the HXR source. A localized enhancement of the reconnection rate corresponds to the position of the HXR source.

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