Explosive events, magnetic reconnection, and coronal heating

Details Explosive events, magnetic reconnection, and coronal heating Explosive events, magnetic reconnection, and coronal heating

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994adspr..14...13d&link_type=abstract

Advances in Space Research, vol. 14, no. 4, p. (4)13-(4)22

Astronomy and Astrophysics

Astronomy

57

Plasma Heating, Solar Atmosphere, Solar Corona, Solar Flares, Solar Spectra, Magnetic Flux, Plasma Diagnostics, Satellite Observation, Solar Magnetic Field, Solar Wind, Spaceborne Astronomy

Scientific paper

Signatures of explosive events are prominent in transition region spectra where they display exceptionally large velocities (greater than 100 km/s) in small areas (1500 km). Their physical properties, deduced from previous analyses of High Resolution Telescope and Spectrograph (HRTS) spectra and more recent work, are summarized here. It now appears that the explosive events are associated with the process of magnetic cancellation and HRTS data obtained during the most recent rocket flight in 1990 provide direct evidence for this assertion. Flux cancellation, which tends to proceed on time-scales of hours, most likely involves magnetic reconnection in a very bursty manner which explains the small, short-lived explosive events. These reconnection events are part of a larger pattern where small flux elements emerge in the supergranule centers and are transported to the boundaries to continually regenerate the network fields on a timescale of about 8 hours. These timescales are also sufficiently short to account for the energetics of the quiet sun.

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