The multi fluid description of the chromospheric motions
Abstract
The major diagnostics of solar chromosphere comes from spectroscopic observations of different spectral lines, which provide the information about the dynamics of minor ions, using strong lines, associated with them (observed by SOHO, SDO, IRIS etc.). They indicate the variation of temperature with altitude and time. On the other hand, general dynamics of the chromosphere is determined by three main components: electrons, protons and neutral hydrogen atoms (probably sometimes by helium component also). We consider the model, similar to plasma discharge, describing it by the system of three-fluid hydrodynamic equations for partially ionized plasma in the presence of electric and magnetic fields. Our description accounts for the processes of ionization and recombination as well as the dissipation of electric currents. Minor ions and atoms are included into our description as impurities, diffusing in the dominant component's gas. Ionization of minor ions is supposed to happen due to collisions with electrons. To achieve this goal, we have the numerical code, written by Sergiy Shelyag and Linh Le Phuong, which is a multi-dimensional parallel solver of systems of hyperbolic differential equations on an arbitrary Cartesian grid. It has already been configured to solve the systems of hydrodynamic, magneto-hydrodynamic and two-fluid magneto-hydrodynamic (ions + neutrals) equations. The code takes into account ionization, recombination and collisional processes for non-linear simulations of solar partially- and fully-ionized plasmas. Actually we are going to test different properties of the code.
- Publication:
-
SF2A-2018: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics
- Pub Date:
- December 2018
- Bibcode:
- 2018sf2a.conf..469T
- Keywords:
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- chromosphere;
- multi-fluid;
- corona;
- heating