Physics
Scientific paper
Dec 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986nascp2442..143d&link_type=abstract
In NASA. Goddard Space Flight Center Coronal and Prominence Plasmas p 143-147 (SEE N87-20871 13-92)
Physics
1
Fine Structure, Solar Physics, Solar Prominences, Solar Temperature, Sun, Thermal Stability, Cooling, Heat Transfer, Size (Dimensions), Solar Magnetic Field, Thermodynamics, Time
Scientific paper
The linear thermal stability of a 2D periodic structure (alternatively hot and cold) in a uniform magnetic field is analyzed. The energy equation includes wave heating (assumed proportional to density), radiative cooling and both conduction parallel and orthogonal to magnetic lines. The equilibrium is perturbed at constant gas pressure. With parallel conduction only, it is found to be unstable when the length scale 1// is greater than 45 Mn. In that case, orthogonal conduction becomes important and stabilizes the structure when the length scale is smaller than 5 km. On the other hand, when the length scale is greater than 5 km, the thermal equilibrium is unstable, and the corresponding time scale is about 10,000 s: this result may be compared to observations showing that the lifetime of the fine structure of solar prominences is about one hour; consequently, our computations suggest that the size of the unresolved threads could be of the order of 10 km only.
Démoulin Pascal
Malherbe Jean-Marie
Raadu Mickael A.
Schmieder Brigitte
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