Reconnection of Twisted Magnetic Flux Tubes as a Solar Flare Mechanism

Details Reconnection of Twisted Magnetic Flux Tubes as a Solar Flare Mechanism Reconnection of Twisted Magnetic Flux Tubes as a Solar Flare Mechanism

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sp42a11l&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SP42A-11

Astronomy and Astrophysics

Astrophysics

7500 Solar Physics, Astrophysics, And Astronomy, 7509 Corona, 7519 Flares, 7524 Magnetic Fields

Scientific paper

The collision and reconnection of magnetic flux tubes in the solar corona is often proposed as a mechanism for solar flares. We study this process by simulating the collision of pairs of twisted flux tubes with a massively parallel collocation viscoresistive MHD code using up to 256 x 256 x 256 Fourier modes. Our aim is to investigate the energy release and the possible global topological changes which occur in flux tube reconnection. We have performed a number of simulations for different angles between the colliding flux tubes and for either co- or counter-helicity flux tubes. We find the following four classes of reconnection can occur: 1) bounce (no appreciable reconnection), 2) merge, 3) slingshot (the classical reconnection picture), and 4) tunnel (a double reconnection). We will describe these four classes of flux tube reconnection, discuss in what range of parameter space each class occurs, and discuss the implications our results have for models of flares. This work was supported by an NRC/NRL Postdoctoral Fellowship, the NASA SECTP, and a grant of computer time from the DoD/HPC Program.

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