title: ÐÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ðµ ÑÐ¾Ð½ÐºÐ¾Ð¹ Ð²ÑÐµÐ¼ÐµÐ½Ð½Ð¾Ð¹ ÑÑÑÑÐºÑÑÑÑ ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ Ð²ÑÐ¿ÑÑÐµÐº Ð² Ð¶ÑÑÑÐºÐ¾Ð¼ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ð¼ Ð´Ð¸Ð°Ð¿Ð°Ð·Ð¾Ð½Ðµ Ð¿Ð¾ Ð´Ð°Ð½Ð½ÑÐ¼ ÑÐºÑÐ¿ÐµÑÐ¸Ð¼ÐµÐ½ÑÐ° ÐÐ¾Ð½ÑÑ-ÐÐ¸Ð½Ð´
title: Ð²ÑÐ¿ÑÑÐºÐ½Ð°Ñ ÐºÐ²Ð°Ð»Ð¸ÑÐ¸ÐºÐ°ÑÐ¸Ð¾Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð±Ð°ÐºÐ°Ð»Ð°Ð²ÑÐ°
titleType: Subtitle
title: Investigation of the fine temporal structure of solar flares in the hard X-ray range according to the KONUS-WIND experiment
Creators: name: ÐÑÐ·ÑÐ¼Ð¸Ð½Ð°, ÐÐ½Ð°ÑÑÐ°ÑÐ¸Ñ
Publisher: name: Ð¡Ð°Ð½ÐºÑ-ÐÐµÑÐµÑÐ±ÑÑÐ³ÑÐºÐ¸Ð¹ Ð¿Ð¾Ð»Ð¸ÑÐµÑÐ½Ð¸ÑÐµÑÐºÐ¸Ð¹ ÑÐ½Ð¸Ð²ÐµÑÑÐ¸ÑÐµÑ ÐÐµÑÑÐ° ÐÐµÐ»Ð¸ÐºÐ¾Ð³Ð¾
Year: 2022
Subjects: ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÐµ Ð²ÑÐ¿ÑÑÐºÐ¸
Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð¾Ðµ Ð¿ÐµÑÐµÑÐ¾ÐµÐ´Ð¸Ð½ÐµÐ½Ð¸Ðµ
Ð¶ÐµÑÑÐºÐ¾Ðµ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ðµ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ðµ
Ð°Ð¿Ð¿ÑÐ¾ÐºÑÐ¸Ð¼Ð°ÑÐ¸Ñ ÑÐ¿ÐµÐºÑÑÐ¾Ð²
solar flares
magnetic reconnectivity
hard X-ray
spectrum approximation
XSPEC
KONUS-WIND

description: Ð¢ÐµÐ¼Ð° Ð²ÑÐ¿ÑÑÐºÐ½Ð¾Ð¹ ÐºÐ²Ð°Ð»Ð¸ÑÐ¸ÐºÐ°ÑÐ¸Ð¾Ð½Ð½Ð¾Ð¹ ÑÐ°Ð±Ð¾ÑÑ: Â«ÐÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ðµ ÑÐ¾Ð½ÐºÐ¾Ð¹ Ð²ÑÐµÐ¼ÐµÐ½Ð½Ð¾Ð¹ ÑÑÑÑÐºÑÑÑÑ ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ Ð²ÑÐ¿ÑÑÐµÐº Ð² Ð¶ÑÑÑÐºÐ¾Ð¼ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ð¼ Ð´Ð¸Ð°Ð¿Ð°Ð·Ð¾Ð½Ðµ Ð¿Ð¾ Ð´Ð°Ð½Ð½ÑÐ¼ ÑÐºÑÐ¿ÐµÑÐ¸Ð¼ÐµÐ½ÑÐ° KONUS-WINDÂ». ÐÑÐµÐ´Ð¼ÐµÑ Ð²ÑÐ¿ÑÑÐºÐ½Ð¾Ð¹ ÐºÐ²Ð°Ð»Ð¸ÑÐ¸ÐºÐ°ÑÐ¸Ð¾Ð½Ð½Ð¾Ð¹ ÑÐ°Ð±Ð¾ÑÑ: ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÐµ Ð²ÑÐ¿ÑÑÐºÐ¸. ÐÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ðµ ÑÐ¾Ð»Ð½ÐµÑÐ½Ð¾Ð¹ Ð°ÐºÑÐ¸Ð²Ð½Ð¾ÑÑÐ¸ Ð¼Ð¾Ð¶ÐµÑ Ð±ÑÑÑ Ð¿ÑÐ¾Ð²ÐµÐ´ÐµÐ½Ð¾ Ð½Ð° ÑÐ°Ð·Ð½ÑÑ Ð¿ÑÐ¾ÑÑÑÐ°Ð½ÑÑÐ²ÐµÐ½Ð½Ð¾-Ð²ÑÐµÐ¼ÐµÐ½Ð½ÑÑ Ð¼Ð°ÑÑÑÐ°Ð±Ð°Ñ. ÐÐ·ÑÑÐµÐ½Ð¸Ðµ ÑÐ¾Ð»Ð½ÐµÑÐ½Ð¾Ð³Ð¾ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð¾Ð³Ð¾ Ð¿Ð¾Ð»Ñ, Ð¿ÑÐ¾ÑÐµÑÑÐ¾Ð² ÑÑÐºÐ¾ÑÐµÐ½Ð¸Ñ Ð¸ ÑÐ°ÑÐ¿ÑÐ¾ÑÑÑÐ°Ð½ÐµÐ½Ð¸Ñ ÑÐ°ÑÑÐ¸Ñ Ð½ÐµÐ¾Ð±ÑÐ¾Ð´Ð¸Ð¼Ð¾ Ð´Ð»Ñ Ð¿Ð¾Ð½Ð¸Ð¼Ð°Ð½Ð¸Ñ Ð¿ÑÐ¾ÑÐµÑÑÐ¾Ð² Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð¾Ð³Ð¾ Ð¿ÐµÑÐµÑÐ¾ÐµÐ´Ð¸Ð½ÐµÐ½Ð¸Ñ. ÐÐ°Ð½Ð½Ð°Ñ ÑÐ°Ð±Ð¾ÑÐ° Ð¿Ð¾ÑÐ²ÑÑÐµÐ½Ð° Ð°Ð½Ð°Ð»Ð¸Ð·Ñ ÑÐ¿ÐµÐºÑÑÐ¾Ð² ÑÐ¾Ð»Ð½ÐµÑÐ½ÑÑ Ð²ÑÐ¿ÑÑÐµÐº Ð² Ð¶ÑÑÑÐºÐ¾Ð¼ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ð¼ Ð´Ð¸Ð°Ð¿Ð°Ð·Ð¾Ð½Ðµ, Ð·Ð°ÑÐµÐ³Ð¸ÑÑÑÐ¸ÑÐ¾Ð²Ð°Ð½Ð½ÑÑ Ñ Ð²ÑÑÐ¾ÐºÐ¸Ð¼ Ð²ÑÐµÐ¼ÐµÐ½Ð½ÑÐ¼ ÑÐ°Ð·ÑÐµÑÐµÐ½Ð¸ÐµÐ¼. ÐÑÑÐ»ÐµÐ´Ð¾Ð²Ð°Ð½Ð¸Ðµ Ð¿ÑÐ¾Ð¸Ð·Ð²Ð¾Ð´Ð¸ÑÑÑ Ð¿Ð¾ Ð´Ð°Ð½Ð½ÑÐ¼ ÑÐºÑÐ¿ÐµÑÐ¸Ð¼ÐµÐ½ÑÐ° KONUS-WIND Ð´Ð»Ñ ÑÐ¾Ð»Ð½ÐµÑÐ½Ð¾Ð¹ Ð²ÑÐ¿ÑÑÐºÐ¸ ÐºÐ»Ð°ÑÑÐ° Ð2, Ð¿ÑÐ¾Ð¸Ð·Ð¾ÑÐµÐ´ÑÐµÐ¹ 26 Ð°Ð¿ÑÐµÐ»Ñ 2003, 00:55:01. Ð Ð¿ÑÐ¾Ð³ÑÐ°Ð¼Ð¼Ðµ XSPEC Ð²ÑÐ¿Ð¾Ð»Ð½ÐµÐ½Ð° Ð°Ð¿Ð¿ÑÐ¾ÐºÑÐ¸Ð¼Ð°ÑÐ¸Ñ Ð¿ÑÐµÐ´Ð²Ð°ÑÐ¸ÑÐµÐ»ÑÐ½Ð¾ Ð¿Ð¾Ð´Ð³Ð¾ÑÐ¾Ð²Ð»ÐµÐ½Ð½ÑÑ ÑÐ¿ÐµÐºÑÑÐ¾Ð² ÑÐ°ÑÑÐ¼Ð°ÑÑÐ¸Ð²Ð°ÐµÐ¼Ð¾Ð¹ ÑÐ¾Ð»Ð½ÐµÑÐ½Ð¾Ð¹ Ð²ÑÐ¿ÑÑÐºÐ¸ Ñ Ð²ÑÐµÐ¼ÐµÐ½Ð½ÑÐ¼ ÑÐ°Ð·ÑÐµÑÐµÐ½Ð¸ÐµÐ¼ 256 Ð¼Ñ Ð¸ Ð±Ð¾Ð»ÐµÐµ Ð³ÑÑÐ±ÑÐ¼ ÑÐ°Ð·ÑÐµÑÐµÐ½Ð¸ÐµÐ¼ â 1024 Ð¼Ñ. ÐÐ¿Ð¿ÑÐ¾ÐºÑÐ¸Ð¼Ð°ÑÐ¸Ñ Ð¿ÑÐ¾Ð¸Ð·Ð²Ð¾Ð´Ð¸ÑÑÑ Ð½Ð° ÑÐ·ÑÐºÐµ Python Ñ Ð¿Ð¾Ð¼Ð¾ÑÑÑ Ð±Ð¸Ð±Ð»Ð¸Ð¾ÑÐµÐº PyXspec, AstroPy, SciPy, MatPlotLib. ÐÑÐ¿Ð¾Ð»ÑÐ·Ð¾Ð²Ð°Ð»Ð¸ÑÑ Ð´Ð²Ðµ ÑÐµÐ½Ð¾Ð¼ÐµÐ½Ð¾Ð»Ð¾Ð³Ð¸ÑÐµÑÐºÐ¸Ðµ Ð¼Ð¾Ð´ÐµÐ»Ð¸: Ð¾Ð´Ð½Ð¾ÑÑÐµÐ¿ÐµÐ½Ð½Ð°Ñ Ð¸ Ð´Ð²ÑÑÑÑÐµÐ¿ÐµÐ½Ð½Ð°Ñ Ñ Ð¸Ð·Ð»Ð¾Ð¼Ð¾Ð¼. ÐÑÐµÐ´Ð¿Ð¾ÑÑÐ¸ÑÐµÐ»ÑÐ½Ð°Ñ Ð¼Ð¾Ð´ÐµÐ»Ñ Ð²ÑÐ±Ð¸ÑÐ°Ð»Ð°ÑÑ Ð¿ÑÐ¸ Ð¿Ð¾Ð¼Ð¾ÑÐ¸ ÐºÑÐ¸ÑÐµÑÐ¸Ñ Ð¤Ð¸ÑÐµÑÐ°. ÐÐ¾ÑÑÑÐ¾ÐµÐ½Ð° Ð²ÑÐµÐ¼ÐµÐ½Ð½Ð°Ñ Ð·Ð°Ð²Ð¸ÑÐ¸Ð¼Ð¾ÑÑÑ Ð´Ð»Ñ Ð¾ÑÐ½Ð¾Ð²Ð½ÑÑ Ð¿Ð°ÑÐ°Ð¼ÐµÑÑÐ¾Ð² Ð¼Ð¾Ð´ÐµÐ»Ð¸ â Ð¿Ð¾ÐºÐ°Ð·Ð°ÑÐµÐ»ÐµÐ¹ ÑÑÐµÐ¿ÐµÐ½Ð¸ ÑÐ¿ÐµÐºÑÑÐ° ÑÐ¾ÑÐ¾Ð½Ð°, Ð·Ð½Ð°ÑÐµÐ½Ð¸Ñ ÑÐ½ÐµÑÐ³Ð¸Ð¸ Ð¸Ð·Ð»Ð¾Ð¼Ð° Ð¸ Ð°Ð¼Ð¿Ð»Ð¸ÑÑÐ´Ñ. ÐÐ¾ Ð¿Ð¾Ð»ÑÑÐµÐ½Ð½ÑÐ¼ Ð´Ð°Ð½Ð½ÑÐ¼ Ð²ÑÐ¿Ð¾Ð»Ð½ÐµÐ½Ð° Ð¾ÑÐµÐ½ÐºÐ° ÑÐ¿ÐµÐºÑÑÐ°Ð»ÑÐ½Ð¾Ð¹ ÑÐ²Ð¾Ð»ÑÑÐ¸Ð¸. Ð ÐµÐ·ÑÐ»ÑÑÐ°ÑÑ ÑÐ°Ð±Ð¾ÑÑ Ð¿Ð¾ÐºÐ°Ð·Ð°Ð»Ð¸, ÑÑÐ¾ Ð²ÑÐµÐ¼ÐµÐ½Ð½Ð¾Ð¹ Ð¼Ð°ÑÑÑÐ°Ð± Ð¿ÐµÑÐµÐ¼ÐµÐ½Ð½Ð¾ÑÑÐ¸ Ð¶ÑÑÑÐºÐ¾Ð³Ð¾ ÑÐµÐ½ÑÐ³ÐµÐ½Ð¾Ð²ÑÐºÐ¾Ð³Ð¾ Ð¸Ð·Ð»ÑÑÐµÐ½Ð¸Ñ Ð´Ð°Ð½Ð½Ð¾Ð¹ ÑÐ¾Ð»Ð½ÐµÑÐ½Ð¾Ð¹ Ð²ÑÐ¿ÑÑÐºÐ¸ ÑÐ¾ÑÑÐ°Ð²Ð»ÑÐµÑ 1 ÑÐµÐºÑÐ½Ð´Ñ. Ð¢Ð°ÐºÐ¶Ðµ Ð±ÑÐ»Ð¾ Ð¿Ð¾Ð»ÑÑÐµÐ½Ð¾ Ð¾Ð³ÑÐ°Ð½Ð¸ÑÐµÐ½Ð¸Ðµ Ð½Ð° Ð¿Ð°ÑÐ°Ð¼ÐµÑÑÑ ÑÑÐºÐ¾ÑÐµÐ½Ð¸Ñ ÑÐ»ÐµÐºÑÑÐ¾Ð½Ð¾Ð² Ð¿ÑÐ¸ Ð¼Ð°Ð³Ð½Ð¸ÑÐ½Ð¾Ð¼ Ð¿ÐµÑÐµÑÐ¾ÐµÐ´Ð¸Ð½ÐµÐ½Ð¸Ð¸.
description: Topic of the final qualification work: "Investigation of the fine temporal structure of solar flares in the hard X-ray range according to the KONUS-WIND experiment. "The subject of the final qualifying work: solar flares. The study of solar activity can be carried out on different space-time scales. The study of the solar magnetic field, the processes of acceleration and propagation of particles is necessary for understanding the processes of magnetic reconnection. This work is devoted to the analysis of the spectra of solar flares in the hard X-ray range, recorded with a high temporal resolution.Â  The study is based on data from the KONUS-WIND experiment for an M2 class solar flare on April 26, 2003, 00:55:01. The previously prepared spectra of the considered solar flare were fitted in the XSPEC package with a time resolution of 256 ms and 1024 ms. Fitting was performed in Python using the PyXspec, AstroPy, SciPy, MatPlotLib libraries. Two phenomenological models were used:Â  a power law and a and a broken power law model. The preferred model was selected using the Fisher criterion.A time dependence is constructed for the main parameters of the model - the power law indices, the value of the break energy and the amplitude. Based on the obtained data, the time scale of the spectral evolution was estimated.The results of the work showed that the time scale of the variability of the hard X-ray emission of this solar flare is 1 seconds. A constraint on the parameters of electron acceleration during magnetic reconnection was also obtained.