Current sheet models for solar prominences. II - Energetics and condensation process

Details Current sheet models for solar prominences. II - Energetics and condensation process Current sheet models for solar prominences. II - Energetics and condensation process

Oct 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...127..153m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 127, no. 1, Oct. 1983, p. 153-160.

Astronomy and Astrophysics

Astrophysics

11

Astronomical Models, Current Sheets, Plasma Dynamics, Solar Prominences, Dynamic Models, Solar Corona, Thermal Instability

Scientific paper

A steady state dynamic model for solar prominences of the Kuperus and Raadu type was previously proposed by Malherbe and Priest (1983), but only the motion through series of quasi-static states was investigated there. The mechanisms for formation, condensation and cooling of plasma in this model are studied. As hot coronal material approaches the filament sheet, it is expected to cool and condense. Cold material is then carried up through the prominence by rising magnetic field lines due to converging photospheric motions below the filament. Two possible ways are suggested of triggering a thermal instability and so producing such a stationary condensation process: a larger pressure in the sheet, or a smaller wave heating in the reconnected field than in the surrounding corona. This paper presents a simple model to simulate the plasma condensation: the thermodynamics of the cooling process, as well as the dynamics of new material entering the prominence sheet, are described in detail.

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