Б а с р е д а к т о р ы ф.-м.ғ.д., проф., ҚР ҰҒА академигі Ғ.М. Мұтанов Р е д а к ц и я а л қ а с ы: Жұмаділдаев А.С. проф., академик (Қазақстан) Кальменов Т.Ш. проф., академик (Қазақстан) Жантаев Ж.Ш. проф., корр.-мүшесі (Қазақстан) Өмірбаев У.У. проф. корр.-мүшесі (Қазақстан) Жүсіпов М.А. проф. (Қазақстан) Жұмабаев Д.С. проф. (Қазақстан) Асанова А.Т. проф. (Қазақстан) Бошкаев К.А. PhD докторы (Қазақстан) Сұраған Д. корр.-мүшесі (Қазақстан) Quevedo Hernando проф. (Мексика), Джунушалиев В.Д. проф. (Қырғыстан) Вишневский И.Н. проф., академик (Украина) Ковалев А.М. проф., академик (Украина) Михалевич А.А. проф., академик (Белорус) Пашаев А. проф., академик (Əзірбайжан) Такибаев Н.Ж. проф., академик (Қазақстан), бас ред. орынбасары Тигиняну И. проф., академик (Молдова) «ҚР ҰҒА Хабарлары. Физика-математикалық сериясы».

Б а с р е д а к т о р ы ф.-м.ғ.д., проф., ҚР ҰҒА академигі Ғ.М. Мұтанов Р е д а к ц и я а л қ а с ы: Жұмаділдаев А.С. проф., академик (Қазақстан) Кальменов Т.Ш. проф., академик (Қазақстан) Жантаев Ж.Ш. проф., корр.-мүшесі (Қазақстан) Өмірбаев У.У. проф. корр.-мүшесі (Қазақстан) Жүсіпов М.А. проф. (Қазақстан) Жұмабаев Д.С. проф. (Қазақстан) Асанова А.Т. проф. (Қазақстан) Бошкаев К.А. PhD докторы (Қазақстан) Сұраған Д. корр.-мүшесі (Қазақстан) Quevedo Hernando проф. (Мексика), Джунушалиев В.Д. проф. (Қырғыстан) Вишневский И.Н. проф., академик (Украина) Ковалев А.М. проф., академик (Украина) Михалевич А.А. проф., академик (Белорус) Пашаев А. проф., академик (Əзірбайжан) Такибаев Н.Ж. проф., академик (Қазақстан), бас ред. орынбасары Тигиняну И. проф., академик (Молдова) «ҚР ҰҒА Хабарлары. Физика-математикалық сериясы».

We observed top 10 X-class solar flares registered in the period November 1997 - September 2017. We measure physical parameters of 10 solar flares, such as the temporal scale, size, and magnetic flux density, and find that the sizes of flares tend to be distributed more broadly as the GOES class becomes weaker and that there is a lower limit of magnetic flux density that depends on the GOES class. We also made a brief analysis of solar flares registered in these days, also has shown the duration of time and peak of solar flares in Universal time. We have identified several physical quantities of solar flares and estimated reconnection rate of solar flares. To determine the physical parameters we used images taken with the AIA instrument on board SDO satellite at wavelengths 131 Å, 174 Å, 193 Å, 211 Å, 335 Å, 1600 Å, 1700 Å, 4500 Å, SXT - pictures, HMI Magnetogram, SOLIS Chromospheric Magnetogram, GOES XRT-data. We estimate reconnection inflow velocity, coronal Alfven velocity, and reconnection rate using the observed values. The inflow velocities are distributed from a few km s-1 to several tens of km s-1, and the Alfven velocities in the corona are in the range from 103 to 104 km s-1. Hence, the reconnection rate is 10-3. We find that the reconnection rate in a flare tends to decrease as the GOES class of the flare increases.

Solar flares are strong radiation bursts, whereas large clouds of solar material and magnetic fields that erupt at high speeds from the Sun are coronal mass ejections. Harmful radiation from a flare does not pass through the atmosphere of the Earth to physically impact humans on the ground, but can disrupt the atmosphere in the layer where GPS and communication signals travel. Flares generate results across the entire electromagnetic spectrum. They emit x-rays and ultraviolet radiation, which means extremely high temperatures during a flash. Radio waves mean that tiny fractions of particles are accelerated to high levels of energy. Most of the radiation is synchrotron radiation produced along magnetic field lines by electrons traveling along spiral paths. In this paper was monitored solar flare registered on February 25, 2015. This flare, which peaked at 00:49 am EDT from a sunspot called Active Region 1990 (AR1990), is classified as an X4.9-class flare. We have performed solar data analysis using the Python/SunPy tool. SunPy was chosen as the principle data analysis environment since it provides easy to use interfaces to the Virtual Solar Observatory (VSO).

Solar-based flares are one of the most impressive energetic events in the solar atmosphere. Given their part of job in the solar corona's energy balance and their function playing important role in the space weather, numerous observations researched the release of energy and induction of solar flares, focusing on the solar active. National solar observatories are providing the overall network with a wealth of data, covering extensive time ranges (e.g. Solar and Heliospheric Observatory, SOHO), numerous perspectives (Solar Terrestrial Relations Observatory, STEREO), and returning a lot of information (Solar Dynamics Observatory, SDO). Specifically, the huge amount of SDO data are accessible only from a few repositories, such type of data as a full-cadence data or full-disk of scientific concern are hard to download, because of their size. To address these difficulties we have begun to build up a new solar application using the Java programming language for a stand-alone application type (GUI).