Magnetic reconnection in numerical simulations of the Bastille day flare

Details Magnetic reconnection in numerical simulations of the Bastille day flare Magnetic reconnection in numerical simulations of the Bastille day flare

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh43a1925v&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH43A-1925

Astronomy and Astrophysics

Astrophysics

[7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7526] Solar Physics, Astrophysics, And Astronomy / Magnetic Reconnection, [7549] Solar Physics, Astrophysics, And Astronomy / Ultraviolet Emissions

Scientific paper

If neither waves nor adiabatic heating due to compression are taken into account, coronal heating may be obtained in numerical simulations from current dissipation inside solar flares. To increase Joule heating locally we used a model for hyper resistivity (Klimas et al., 2004: Journal of Geophysical Research, 109, 2218-2231). Here the change in resistivity is due to small scale (less than 1Mm in our simulations) current density fluctuations. Whenever the current exceeds a cut-off value, magnetic resistivity jumps sharply to reach a maximum locally thus increasing magnetic gradients at the border of the flare. In this way, not only the current increases but also the maximum is slowly displaced and simulations of the full set of 3-D MHD equations show a progression westward as can be seen in SOHO-EIT images of the ''slinky''. In our simulations of the Bastille day flare, most of the reconnection events take place just above the transition and mostly follow the neutral line but it is Spitzer thermal diffusivity together with radiative cooling that illuminates magnetic arcades in a way similar to what can be seen in extreme ultra-violet animations of the slinky.

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