Fluid motions in the solar atmosphere. I - On the origin and decay of spicules. II - A spicule model with emission lines

Details Fluid motions in the solar atmosphere. I - On the origin and decay of spicules. II - A spicule model with emission lines Fluid motions in the solar atmosphere. I - On the origin and decay of spicules. II - A spicule model with emission lines

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...266..537c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 266, no. 1, p. 537-559.

Computer Science

Numerical Analysis

29

Solar Atmosphere, Spicules, Adiabatic Conditions, Chromosphere, Conductive Heat Transfer, Hydrodynamic Equations, Numerical Analysis, Solar Corona, Solar Radiation

Scientific paper

A time-dependent numerical method including the effects of radiation, thermal conduction, mechanical heating, and ionization of hydrogen is employed to investigate the origin and decay of solar spicules. The initial atmosphere is a realistic stationary solar atmosphere, the transition region of the chromosphere, and the corona is treated as a continuous layer. It is shown that a spicule could be regarded as the matter which follows behind the chromosphere-corona transition region, which is pushed upward into the corona by an impulsive wave event. The spicule declines gradually and shows recurrent behavior due to the radiative loss and the oscillation of the atmosphere. Solar spicules are simulated using MGII k and H Ly-alpha line emissions as a radiative cooling mechanism in the chromosphere and low transition region. It is shown that the inclusion of the line emission greatly improves the time-dependence and the physical behavior of the spicule model.

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