A shock condensation mechanism for loop prominences

Details A shock condensation mechanism for loop prominences A shock condensation mechanism for loop prominences

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...302l..67f&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 302, March 15, 1986, p. L67-L70. Research supported

Astronomy and Astrophysics

Astrophysics

78

Coronal Loops, Solar Flares, Solar Prominences, Condensation, Magnetohydrodynamics, Shock Waves, Stellar Models

Scientific paper

Self-consistent, numerical solutions of the resistive MHD equations in two dimensions show that a quasi-stationary, fast-mode shock is a characteristic feature of the reconnection dynamics of the Kopp-Pneuman model of two-ribbon flares. A preliminary analysis of the effects of radiative cooling and thermal conduction suggests that the fast shock can help trigger a thermal condensation (i.e., a loop prominence) if the reconnecting magnetic fields are sufficiently strong.

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