Mass upflows in 'post'-flare loops

Details Mass upflows in 'post'-flare loops Mass upflows in 'post'-flare loops

Oct 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...88..211f&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 88, Oct. 1983, p. 211-218. Research supported by the Science and Engineering Research Counc

Physics

15

Coronal Loops, Magnetic Field Configurations, Magnetohydrodynamic Flow, Solar Flares, Solar Magnetic Field, Particle Acceleration, Pressure Distribution, Solar Corona, Stellar Models

Scientific paper

A self-consistent numerical model of a reconnecting magnetic field configuration similar to that occurring during the main-phase of two-ribbon flares is used to estimate the upflow caused by the fast-mode expansion of the magnetic field moving into the reconnection region. Such an expansion creates a field-aligned pressure gradient which accelerates plasma upward from the chromospheric base of magnetic field lines in the region external to the loops. The numerical results imply that the amount of mass sucked up in this way is even smaller than was previously estimated by Kopp and Pneuman who used a kinematic model. Therefore, some indirect mechanism (such as evaporation), which would probably derive its motive power from the thermal energy generated by the reconnection, is required to explain the large mass upflows inferred from observations.

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