Large-Scale Magnetostatic Structures in the Solar Corona and a Model of the Polar Coronal Hole
- 3 Downloads
A method for the theoretical calculation of large-scale magnetoplasma solar coronal structures with a rotational symmetry in the spherical coordinate system is presented. The method makes it possible to obtain analytical solutions for equilibrium spatial distributions of pressures, densities, and temperatures in any preset axisymmetrical magnetic configuration. The obtained solution is used to plot model polar coronal holes via the introduction of a small power correction in the force free distribution of the magnetic field for subpolar region. The thermodynamic parameters of the coronal hole represented in this model are close to the observed values.
The study was partially supported by the Program of the Presidium of the Russian Academy of Sciences P-28 (Experimental and Theoretical Exploration of Objects of the Solar System and Stellar Planetary Systems subprogram) and the Russian Foundation for Basic Research, project no. 18-02-00168 and the Russian Science Foundation, project no. 15-12-20001.
- 1.Munro, R.H. and Jackson, B.V., Physical properties of a polar coronal hole from 2 to 5 solar radii, Astrophys. J., 1977, pp. 874, 875, 877–886.Google Scholar
- 5.Solov’ev, A.A., Korolkova, O.A., and Kirichek, E.A., Model of quiescent prominence with the helical magnetic field, Geomagn. Aeron., 2016, no. 8, pp. 1090–1094.Google Scholar
- 6.Korolkova, O.A. and Solov’ev, A.A., Modeling of the fine filament structure of quiescent solar prominences, Geomagn. Aeron. (Engl. Transl.), 2017, no. 8, pp. 1018–1022.Google Scholar