Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999esasp.446..457m&link_type=abstract
8th SOHO Workshop: Plasma Dynamics and Diagnostics in the Solar Transition Region and Corona. Proceedings of the Conference hel
Astronomy and Astrophysics
Astrophysics
Scientific paper
Solar prominences and filaments are observed to consist of a collection of small H-alpha condensations or knots. We address two key issues concerning these condensations: (1) the mechanism for their formation, and (2) the origin of their observed motions. Recently, Zirker, Martin and co-workers have found that filament condensations appear to move approximately horizontally with velocities of order 5 - 10 km/s. These observations provide important constraints on the magnetic structure of prominences. We propose that the condensations form due to a lack of thermal equilibrium in the magnetic flux tubes threading through the prominence corona. We use LOOPAMR a new 1D high-order Godunov code that includes both thermal conduction and radiation with PARAMESH, a fully adaptive mesh refinement tool, to simulate for the first time the complete formation process of a prominence condensation. We show that both the origin and the observed velocities are explained by our model. In addition we discuss the implication of our model for coronal heating and for the global structure of prominences.
Antiochos Spiro
MacNeice Peter
Spicer Daniel S.
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