Abstract
The M7.7 solar flare on July 19, 2012, is the most dramatic example of a “Masuda” flare with a well-defined second X-ray above-the-loop-top source. The behavior of the system of loops accompanying this flare has been studied comprehensively by Liu et al. based on Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) and Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) data. We have performed spectroscopic and filter observations of the Hα loops in this flare with the Large Solar Vacuum Telescope. The basic physical parameters in the loops of this peculiar flare generally coincide with the known data in Hα loops. However, the electron density, 1011 cm−3, and the integrated disk-center continuum intensity, 12%, are quite high, given that the observations were obtained almost 3 h after the flare onset.We have estimated the ascending velocity of the loop arcade (~3.5 km s−1) and the height difference between the Hα and 94 Å loops (~2 × 104 km).
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Original Russian Text © N.M. Firstova, V.I. Polyakov, 2017, published in Pis’ma v Astronomicheskii Zhurnal, 2017, Vol. 43, No. 11, pp. 845–856.
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Firstova, N.M., Polyakov, V.I. Structure and physical conditions in the Hα loops of an M7.7 solar flare. Astron. Lett. 43, 768–779 (2017). https://doi.org/10.1134/S1063773717110032
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DOI: https://doi.org/10.1134/S1063773717110032