Advertisement

Geomagnetism and Aeronomy

, Volume 58, Issue 7, pp 953–958 | Cite as

Large-Scale Magnetostatic Structures in the Solar Corona and a Model of the Polar Coronal Hole

  • O. A. Korolkova
  • A. A. Solov’ev
Article

Abstract

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.

Notes

ACKNOWLEDGMENTS

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.

REFERENCES

  1. 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
  2. 2.
    Zirker, J.B., Coronal holes and high-speed wind streams, Rev. Geophys. Space Phys., 1977, vol. 15, pp. 257–269.CrossRefGoogle Scholar
  3. 3.
    Obridko, V.N. and Solov’ev, A.A., Magnetohydrostatic model for a coronal hole, Astron. Rep., 2011, vol. 55, pp. 1144–1155.CrossRefGoogle Scholar
  4. 4.
    Hahn, M. Bryans, P., Landi, E., et al., Properties of a polar coronal hole during solar minimum in 2007, Astrophys. J., 2010, vol. 725, no. 1, pp. 774–786.CrossRefGoogle Scholar
  5. 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. 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
  7. 7.
    Low, B.C., On the large-scale magnetostatic coronal structures and their stability. Astrophys. J., 1984, vol. 286, pp. 772–786.CrossRefGoogle Scholar
  8. 8.
    Solov’ev, A.A., The structure of solar filaments, Astron. Rep., 2010, vol. 54, pp. 86–95.CrossRefGoogle Scholar
  9. 9.
    Solov’ev, A.A. and Kirichek, E.A., Magnetohydrostatics of a vertical flux tube in the solar atmosphere: Coronal loops, a model of a ring flare filament, Astron. Lett., 2015, vol. 41, pp. 211–224.CrossRefGoogle Scholar
  10. 10.
    Avrett, E.H. and Loeser, R., Models of the solar chromosphere and transition region from SUMER and HRTS observations: Formation of the extreme-ultraviolet spectrum of hydrogen, carbon, and oxygen, Astrophys. J. Suppl. Ser., 2008, vol. 175, pp. 229–276.CrossRefGoogle Scholar

Copyright information

© Pleiades Publishing, Ltd. 2018

Authors and Affiliations

  1. 1.Central (Pulkovo) Astronomical Observatory, Russian Academy of SciencesSt. PetersburgRussia
  2. 2.Кalmyk State UniversityElistaRussia

Personalised recommendations