Flare June 7, 2011, and analysis of eruptive prominence fragments

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Abstract

Solar flares can be accompanied by high plasma velocities exceeding several hundred km/s. Detection and measurement of such velocities is limited by narrow-band and small wavelength range in most solar instruments. However, similar events with Doppler velocities exceeding two hundred km/s have been detected by the solar optical spectrographs at the Ondřejov Observatory. We present the results of the analysis of our multi-wavelength observations performed during the solar flare of June 7, 2011 and the calculation of several physical parameters of the eruptive prominence fragments following the flare. The calculation of the radiation of heated gas are performed taking into account self-absorption in the spectral lines of hydrogen and calcium. All the crucial processes of discrete level populating and depopulating are taken into account in the balance equations. The theoretical radiation fluxes in the lines coincide with those observed in the temperature range of 6300–10000 K at a gas concentration of about (3–5) × 1010 см–3 , a gas layer thickness of 6800–7000 km and a column density of (2–4) × 1019 см–2 .

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About the authors

Yu. A. Kupryakov

Lomonosov Moscow State University, Sternberg Astronomical Institute

Author for correspondence.
Email: kupry@asu.cas.cz
Russian Federation, Moscow

K. V. Bychkov

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: kupry@asu.cas.cz
Russian Federation, Moscow

V. A. Maliutin

Lomonosov Moscow State University

Email: kupry@asu.cas.cz

Faculty of Physics

Russian Federation, Moscow

A. B. Gorshkov

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: kupry@asu.cas.cz
Russian Federation, Moscow

O. M. Belova

Lomonosov Moscow State University

Email: kupry@asu.cas.cz

Faculty of Physics

Russian Federation, Moscow

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Supplementary files

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2. Fig. 1. GOES15 X-ray flux [W/m2]. The gray curve corresponds to the range 1–8 Å, the black curve to the range 0.5–4 Å.

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3. Fig. 2. On the left is the SDO filtergram in the 304 Å line. The white vertical line corresponds to the position of the spectrograph slit. On the right is the Hα spectrum (MFS Ondřejov). Observation time: 06:40:32 UT.

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4. Fig. 3. View of the falling fragment in the Hα line. The distance between the horizontal reference lines corresponds to 5 × 104 km.

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5. Fig. 4. An example of determining the radiation flux in the Hα line. The shaded part corresponds to the flux from the “luminous” fragment of the ejecta.

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