Dynamical magnetic reconnection in Parker's coronal heating model

Details Dynamical magnetic reconnection in Parker's coronal heating model Dynamical magnetic reconnection in Parker's coronal heating model

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997adspr..19.1865v&link_type=abstract

Advances in Space Research, vol. 19, p. 1865

Astronomy and Astrophysics

Astronomy

Solar Corona, Magnetic Field Reconnection, Solar Heating, Coronal Loops, Plasma Dynamics, Solar Magnetic Field, Astronomical Models, Digital Simulation, Photosphere, Magnetic Flux

Scientific paper

Parker's (1994) loop-heating model is presently numerically simulated in order to investigate dynamics and global power balance; an assessment is thus made of the model's viability as a candidate for coronal heating. The results obtained for the small-scale dynamics of coronal loops suggest that photospheric granular motions quasi-statically twist the magnetic field of the corona in random-walk fashion; the perpendicular magnetic energy increases, and magnetic shear builds up at the quasi-separatrices of the resulting close-packed magnetic flux tubes.

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