The gradual and impulsive reconnection and the preheating of solar flares

Details The gradual and impulsive reconnection and the preheating of solar flares The gradual and impulsive reconnection and the preheating of solar flares

Sep 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987soph..107..271l&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 107, no. 2, 1987, p. 271-282.

Physics

9

Coronal Loops, Magnetic Field Reconnection, Magnetic Flux, Solar Flares, Current Density, Light Curve, Magnetic Fields, Solar X-Rays, Ultraviolet Radiation

Scientific paper

The preheating phase of solar flares triggered by emerging magnetic flux is discussed. The development of microinstabilities in the diffusion region during the emergence process is considered, and four different types of reconnection as well as the impulsive phase of flares are proposed. It is found that during the emergence of new magnetic flux the current sheet will not 'jump' from the initial classical state to a fully turbulent one, but will remain in a marginally turbulent state which may develop either gradually or impulsively depending on the conditions of emergence. As a consequence of this, it is found that four cases of reconnection are indeed possible: a weak gradual heating, a weak impulsive process, a gradual preheating followed by an impulsive phase, and violent bursty reconnection. The expansion rate of the diffusion region, the duration of the gradual phase, the magnetic energy release, and the energy deposition rate in coronal loops during the gradual phase are derived under simplifying assumptions and applied to X-ray and UV observations of flares from the Solar Maximum Mission.

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