Simulation of spectral observations of an eruptive prominence

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Abstract

The paper presents the results of an analysis of observations of an eruptive prominence on the MFS and HSFA2 spectrographs of the Ondřejov Observatory (Astronomical Institute, Czech Republic) in the lines of hydrogen, helium and calcium. After processing the spectra, the integral radiation fluxes in the lines were determined and a theoretical calculation of the physical parameters of the plasma was carried out using a model in the absence of local thermodynamic equilibrium. A comparison of the observed and calculated values showed that the observed radiation fluxes in the lines can be explained in a model of stationary gas radiation taking into account the opacity in the spectral lines. To calculate theoretical fluxes, in some cases it was necessary to introduce radiation from several layers with different temperatures and heights. The calculated radiation fluxes agree with the observed ones with an accuracy of 10%. As a result of the simulation, the main parameters of the prominence plasma were obtained: temperature, concentration, etc. The values of radiation fluxes in the spectral lines indicate the inhomogeneity of the emitting gas, and there may be regions next to each other whose temperatures differ by an order of magnitude.

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About the authors

Yu. A. Kupryakov

ASCR; Moscow State University

Email: jurij.kupriakov@asu.cas.cz

Astronomical Institute, Sternberg Astronomical Institute

Czech Republic, Ondřejov; Russia, Moscow

K. V. Bychkov

Moscow State University

Email: bychkov@sai.msu.ru

Sternberg Astronomical Institute

Russian Federation, Moscow

O. M. Belova

Moscow State University

Email: whitecanvas05122010@mail.ru

Sternberg Astronomical Institute

Russian Federation, Moscow

A. B. Gorshkov

Moscow State University

Email: gorshkov@sai.msu.ru

Sternberg Astronomical Institute

Russian Federation, Moscow

P. Kotrč

ASCR

Author for correspondence.
Email: pavel.kotrc@asu.cas.cz

Astronomical Institute

Czech Republic, Ondřejov

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Supplementary files

Supplementary Files
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1. JATS XML
2. Fig. 1. Hα spectrum at 13:21:11 UT (left). The numbers correspond to photometric sections. Below is the speed scale. In the center is the image on the slit in the Hα line. On the right is an image of SDO 304 Å with the spectrograph slit position and Doppler velocity components marked.

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3. Fig. 2. Filtergram and spectrum in the Hα line at 13:27:40 UT.

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4. Fig. 3. Radiation flux (shaded area) in the Hα line at 13:27:40 UT.

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