Observational Prediction of High Magnetic Reynolds Number Pre-flare Reconnection Events: An Application of Nitta's Self-similar Reconnection Model

Details Observational Prediction of High Magnetic Reynolds Number Pre-flare Reconnection Events: An Application of Nitta's Self-similar Reconnection Model Observational Prediction of High Magnetic Reynolds Number Pre-flare Reconnection Events: An Application of Nitta's Self-similar Reconnection Model

Aug 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010apj...719.1828n&link_type=abstract

The Astrophysical Journal, Volume 719, Issue 2, pp. 1828-1843 (2010).

Astronomy and Astrophysics

Astronomy

2

Magnetic Reconnection, Magnetohydrodynamics: Mhd, Sun: Corona, Sun: Flares, Sun: Magnetic Topology

Scientific paper

We applied the "self-similar evolutionary model" of magnetic reconnection to simple pre-flare reconnection events driven by flux emergence as the first step in inspecting the realizability of the reconnection events predicted by this model. Previous works paid scant attention to the dependence of the magnetic Reynolds number (R*em) on reconnection events. We aim to clarify how the pre-flare phase of reconnection events in the high R*em range that is frequently encountered in astrophysical applications is observed. We clarify that (1) the time variation of the emission measure distribution strongly depends on R*em, (2) the expected light curve for sufficiently low R*em shows a long lifetime property while that for high R*em shows an impulsive property, and (3) in the case of recurrent small reconnection events on the same loop, the released magnetic energy scale is inversely correlated to the rear-end speed of the moving bright point along the loop. Note that other reconnection models cannot totally explain integration of these properties. If evidence of phenomena with these properties can be detected from, e.g., the Hinode observation, it strongly supports the validity of the self-similar reconnection model.

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