Abstract
Based on the measurements of their magnetic fields, solar prominences can be divided into two types: filaments with normal (N) or inverse (I) polarity. In an N-type prominence, the magnetic polarity is the same as in the underlying photosphere, while the opposite polarity occurs in an I-type prominence. This paper continues to develop the method to calculate the pressure, density, and temperature of any given magnetic structure of the configuration. We model the dense and cool prominence with a helical structure of magnetic field. The magnetic configuration under study is introduced in a hydrostatic solar atmosphere given by the model considered by Avrett and Loezer (2008). The presented analytical model describes both the normal-polarity prominences and prominences with inverse polarity.
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Funding
The work was supported by Program KP 19-270 of the Presidium of Russian Academy of Sciences, the Russian Foundation for Basic Research, project no. 18-02-00168, and the Russian Science Foundation, project no. 15-12-20001.
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Translated by N. Semenova
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Korolkova, O.A., Solov’ev, A.A. Structure of Prominences with Normal and Inverse Polarities. Geomagn. Aeron. 59, 858–863 (2019). https://doi.org/10.1134/S0016793219070193
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DOI: https://doi.org/10.1134/S0016793219070193