The dynamical process of a coronal transient associated with an eruptive prominence. I - Basic mechanism

Details The dynamical process of a coronal transient associated with an eruptive prominence. I - Basic mechanism The dynamical process of a coronal transient associated with an eruptive prominence. I - Basic mechanism

May 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..92..373h&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 92, no. 2, May 1983, p. 373-394.

Astronomy and Astrophysics

Astrophysics

9

Plasma Dynamics, Solar Corona, Solar Prominences, Transient Response, Dense Plasmas, Differential Equations, Flow Velocity, Magnetic Flux, Magnetohydrodynamic Flow, Piston Theory, Shock Fronts

Scientific paper

The effects an eruptive solar prominence has on coronal transients are examined analytically in terms of a moving plasma piston. The piston is modeled as an eruptive prominence and/or a magnetic flux feature such as a loop or an arcade travelling ahead of the prominence, the two together driving a shock wave. A rarefied region exists behind the piston and is observed as the dark region of the transient, while the dense area at the front is seen as the bright region. Attention is given to influence of gravity in the directions perpendicular and parallel to the solar gravitational field. The velocity of the shock front is found to be either constant or slightly accelerated. A solution, applicable to the piston region region and the magnetic field, is derived for the MHD equations in the two-dimensional unsteady case. The Lorentz, gravitational, and inertial forces are calculated to be balanced by the pressure gradient. A consistent solution is also found to the gas dynamical equations for two-dimensional, unsteady conditions, and models the region between the piston and the shock wave to satisfy the jump conditions of the front.

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