Numerical hydrodynamics of the jet phenomena in the solar atmosphere. I - Spicules

Details Numerical hydrodynamics of the jet phenomena in the solar atmosphere. I - Spicules Numerical hydrodynamics of the jet phenomena in the solar atmosphere. I - Spicules

Jan 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982soph...75...99s&link_type=abstract

Solar Physics, vol. 75, Jan. 1982, p. 99-118.

Physics

55

Hydrodynamic Equations, Magnetohydrodynamics, Solar Atmosphere, Solar Physics, Spicules, Adiabatic Conditions, Numerical Flow Visualization, Photosphere, Plasma Jets, Shock Wave Generators, Solar Corona

Scientific paper

Constant-cross section, one-dimensional and time-dependent hydrodynamic equations are solved numerically, in the realistic solar atmosphere extending from the photosphere to the corona, in a spicule model for which eruption occurs as a result of sudden pressure enhancement at the bright point located at the root of the spicule. The pressure enhancement generates a shock wave, which becomes stronger as it passes upward through the chromosphere and eventually collides with the chromosphere-corona interface. This interface represents something akin to a contact discontinuity, and the interface begins to move upward as a result of the process outlined. The matter following behind this interface is identified as the solar spicule.

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