Slip running reconnection in the Sun's atmosphere observed by RHESSI, SOHO, TRACE and Hinode

Details Slip running reconnection in the Sun's atmosphere observed by RHESSI, SOHO, TRACE and Hinode Slip running reconnection in the Sun's atmosphere observed by RHESSI, SOHO, TRACE and Hinode

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agusmsh22a..01s&link_type=abstract

American Geophysical Union, Spring Meeting 2007, abstract #SH22A-01

Physics

7519 Flares, 7526 Magnetic Reconnection (2723, 7835)

Scientific paper

Solar double ribbon flares are commonly explained by magnetic field reconnections in the high corona. The bright ribbons, typically observed in Halpha, in EUV with SoHO, TRACE correspond to the ends of the reconnected loops. In most studied cases, the reconnection site is an X-point, where two magnetic separatrices intersect. In this presentation, we show a generalization of this model to 3D complex magnetic topologies where there are no null points, but quasi-separatrices layers instead. In that case, while the ribbons spread away during reconnection, we show that magnetic field lines can quickly slip along them. We propose that this new phenomenon could explain also fast moving HXR footpoints as observed by RHESSI, and that it may be observed in soft X rays with XRT.

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