Abstract
Based on the Paper I (Hu, 1983a), the piston model suggested for the coronal transient. The piston may consist of the eruptive prominence and the preceding compressed magnetic field region, and the moving piston is considered to be the driving source of the coronal transient. There is the compressed flow region ahead the piston and the rarefaction region behind the piston. In this paper, two analytical solutions are discussed in finite regions of piston model.
A consistent solution of the ideal magnetohydrodynamical equations including the gravity is obtained for the two-dimensional unsteady configuration in which density and magnetic field are time dependent. Gravity, Lorentz and inertial forces are balanced by the pressure gradient. The analysis gives a consistent radial velocityu(t) which agrees with the typical velocity of eruptive prominence. The density profile is proportional to 1/r and propagates outward with the velocityu. This solution may be applied to the piston region of moving plasma and magnetic field.
Furthermore, the compressed flow driven by the piston is discussed. The consistent solution of gasdynamical equations including solar gravity is obtained for the unsteady and two-dimensional configuration, which is applied to the region between the piston and shock wave. This solution may satisfy the jump conditions of shock wave, which separates the region of compressed flow and quiet corona.
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Hu, WR. The dynamical process of a coronal transient associated with an eruptive prominence. Astrophys Space Sci 92, 395–415 (1983). https://doi.org/10.1007/BF00651303
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DOI: https://doi.org/10.1007/BF00651303