Non-isothermal magnetohydrostatic equilibrium structure in the solar atmosphere

Details Non-isothermal magnetohydrostatic equilibrium structure in the solar atmosphere Non-isothermal magnetohydrostatic equilibrium structure in the solar atmosphere

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992acasn..33..159h&link_type=abstract

Acta Astronomica Sinica (ISSN 0001-5245), vol. 33, no. 2, p. 159-170.

Other

Equilibrium Equations, Magnetohydrostatics, Solar Activity, Solar Atmosphere, Iterative Solution, Partial Differential Equations, Stellar Models

Scientific paper

The nonisothermal magnetohydrostatic equilibrium is investigated using two-dimensional solutions for the isothermal case. Two models of temperature distribution and two relevant partial differential equations of nonisothermal magnetohydrostatic equilibrium are presented. The equations are solved by an iterative method for appropriate boundary conditions using the isothermal approximation. It is found that the equilibrium configurations change noticeably even with a slight change in temperature. It is suggested that temperature changes may play an important role in increasing solar activity through instability.

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