Observation, Theoretical Calculation and Analysis of the Solar Flare on May 11, 2012

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Solar flare of May 11, 2012 was observed on two spectrographs of the Astronomical Institute of the Czech Academy of Sciences – a multichannel flare spectrograph and a horizontal setup for solar research. After processing the spectra, integral emission fluxes in the hydrogen, helium and calcium lines were determined. Within the framework of the heated gas model, a theoretical calculation of the plasma parameters was performed taking into account the physical conditions in the chromosphere, including self-absorption in the spectral lines. A comparison of six lines at once made it possible to reconstruct the temperature, density and spatial structure of the emitting gas with a high degree of confidence. At the same time, a search for quasi-periodic pulsations in this solar flare was carried out, which showed the absence of such in almost all spectral ranges. An exception is the detection of pulsations in the images of the chromosphere on the spectrograph slit in the Hα line with a period of 30 s.

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作者简介

Yu. Kupryakov

Lomonosov Moscow State University; Astronomical Institute of the Academy of Sciences of the Czech Republic

编辑信件的主要联系方式.
Email: kupry@asu.cas.cz
俄罗斯联邦, Moscow; Ondřejov, Czech Republic

K. Bychkov

Lomonosov Moscow State University

Email: kupry@asu.cas.cz
俄罗斯联邦, Moscow

O. Belova

Lomonosov Moscow State University

Email: kupry@asu.cas.cz
俄罗斯联邦, Moscow

A. Gorshkov

Lomonosov Moscow State University

Email: kupry@asu.cas.cz
俄罗斯联邦, Moscow

V. Malyutin

Lomonosov Moscow State University

Email: malyutinv@list.ru
俄罗斯联邦, Moscow

参考

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2. Fig. 1. The filtergram in the Hα line at 13:07 UT. The vertical line corresponds to the slit of the spectrograph, the two horizontal lines are reference lines and serve to tie the filtergram to the spectra.

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3. Fig. 2. Hα line filtergram (1) and spectra of the H CaII and Hε; Hβ; HeI D3; Hα; Ca IR 8542 Å lines (panels 2-6) at 13:13 UT.

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4. Fig. 3. Example of the variation of the profiles of the H CaII and Hε lines in the time interval 13:03:33-13:14:43 UT, as well as the profile for the quiet Sun.

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5. Fig. 4. Radiation fluxes in spectral lines at selected moments of time.

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6. Fig. 5. Pulsation spectrum determined from chromospheric images in the Hα line. The axes of periods P in minutes and amplitude A in conventional units are given in logarithmic scale. The arrows show: 1 - signal spectrum; 2 - linear regression performed through the signal; 3 - noise level; 4 - 90% significance level.

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7. Fig. 6. Flux spectrum on the spectrograph slit in the Hα line. The solid line indicates the signal spectrum, and the dashed line indicates the significance level of 90% in conventional units. The period axis is given in minutes.

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