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NLTE Model of a Quiescent Filament

Published online by Cambridge University Press:  12 April 2016

E.V. Kononovich ,
A.B. Gorshkov ,
O.B. Smirnova  and
P. Kotrč
E.V. Kononovich
Affiliation:
Sternberg Astronomical Institute, 119899 Moscow, Russia
A.B. Gorshkov
Affiliation:
Sternberg Astronomical Institute, 119899 Moscow, Russia
O.B. Smirnova
Affiliation:
Sternberg Astronomical Institute, 119899 Moscow, Russia
P. Kotrč
Affiliation:
Astronomical Institute, 25165 Ondřejov, Czech Republic

Abstract

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The Sacramento Peak Observatory VTT Echelle Spectrograph was used to obtain high resolution spectrograms of the filament at W06° S27° observed on April 9, 1991 in hydrogen Hα, Hβ, and CaII H and λ 8498 lines. The line profiles were measured and digitized. A numerical code based on the MALI approach with partial frequency redistribution (PRD) in resonance lines was applied to obtain theoretical profiles of hydrogen and CaII lines. As a result of fitting the observed and calculated profiles, the physical parameters of the filament plasma were obtained. They include temperature, gas pressure, electron density and turbulent velocity.

Type
Filaments and Their Environment
Information
International Astronomical Union Colloquium , Volume 167: New Perspectives on Solar Prominences , 1998 , pp. 190 - 195
Copyright
Copyright © Astronomical Society of the Pacific 1998

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