Applying an Automatic Image-Processing Method to Synoptic Observations

Tlatov, A. G.; Vasil'eva, Valeria V.; Makarova, V. V.; Otkidychev, P. A.

doi:10.1007/s11207-013-0404-7

Cited by 32 publications

(17 citation statements)

References 16 publications

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“…Чтобы идентифицировать солнечные пятна на солнечных изображениях, мы использовали методы, опубликованные в программе SolarView [4]. Солнечное изображение может содержать не только элементы, принадлежащие Солнцу, но также и различные артефакты, такие как дефект эмульсии, стирание эмульсии, царапины, пылинки, облака, надписи, пятна, маркеры ориентации и многое другое.…”

Section: метод обработкиunclassified

Creation of Series of Properties of Individual Sunspots

Tlatov¹,

Vasil’eva²,

Sapeshko³

et al. 2019

Proceedings of the 23rd All-Russia Conference on Solar and Solar-Terrestrial Physics

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Section: метод обработкиunclassified

Creation of Series of Properties of Individual Sunspots

Tlatov¹,

Vasil’eva²,

Sapeshko³

et al. 2019

Proceedings of the 23rd All-Russia Conference on Solar and Solar-Terrestrial Physics

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“…Первая вспышка класса M (М1. Магнитографический анализ выполнялся по данным SDO/HMI по методике, описанной в [8]. Вычислялись потоки магнитного поля, локальные горизонтальные градиента магнитного поля в различных частях АО, расстояние между областями максимальных магнитных полей противоположных полярностей, суммарный градиент и положение максимального градиента.…”

Section: Doi: 1031725/0552-5829-2018-15-18unclassified

Evolution of Solar Active Region 12673 by Ratan-600 and Sdo Data

Abramov-Maximov¹,

Observatory²,

Borovik³

et al. 2018

Proceedings of the 22nd All-Russia Conference on Solar and Solar-Terrestrial Physics

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Context: We continue our previous researches of solar active regions (ARs) where strong flares occurred to reveal features indicate that a strong flare is about to take place. Aims: The aim of this paper is to study AR NOAA 12673 on pre-flare phase in the beginning of September 2017. We focus on the behavior of microwave emission and magnetic field structure before the first M-class flare on September 4. Methods: We studied microwave emission and magnetic-field characteristics of AR as based on RATAN-600 and SDO/HMI data. For comparison we considered a well-developed AR NOAA 12674, in which there were only a few weak flares of the C-class. Results: As in the previously investigated cases, we registered a sharp increase of the magnetic field gradient with its decrease directly before the flare and a significant increase of microwave emission before the first M-class flare in NOAA 12673. In NOAA 12674 it was not detected significant changes in the gradient of the magnetic field and microwave radiation. The distance between regions of opposite magnetic polarity decrease initially. Then it begins to increase. On the phase of its increasing the flares occurred. The increase of microwave emission may be interpreted as a result of development of neutral line associated source.

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“…The SDO/HMI data was analyzed with an accumulation time of 45 s at 00:00, 05:00, 10:00, 15:00, and 20:00 UT. Automatic identifying of sunspots and measurement of the magnetic flux in them by SDO/HMI observations in the continuum and in magnetographic observations was used (Tlatov et al, 2014). The method for calculating the index of solar flares used in this paper can be described in the following steps.…”

Section: Magnetographic Investigations Of Ar 12242mentioning

confidence: 99%

Features of Microwave Radiation and Magnetographic Characteristics of Solar Active Region NOAA 12242 Before the X1.8 Flare on December 20, 2014

et al. 2017

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This paper continues the cycle of authors works on the detection of precursors of large flares (M5 and higher classes) in active regions (ARs) of the Sun by their microwave radiation and magnetographic characteristics. Generalization of the detected precursors of strong flares can be used to develop methods for their prediction. This paper presents an analysis of the development of NOAA AR 12242, in which arXiv:1711.09134v1 [astro-ph.SR] 24 Nov 2017 an X1.8 flare occurred on December 20, 2014. The analysis is based on regular multiazimuth and multiwavelength observations with the RATAN-600 radio telescope in the range 1.65-10 cm with intensity and circular polarization analysis and data from the Solar Dynamics Observatory (SDO). It was found that a new component appeared in the AR microwave radiation two days before the X-flare. It became dominant in the AR the day before the flare and significantly decreased after the flare. The use of multiazimuth observations from RATAN-600 and observations at 1.76 cm from the Nobeyama Radioheliograph made it possible to identify the radio source that appeared before the X-flare with the site of the closest convergence of opposite polarity fields near the neutral line in the AR. It was established that the Xflare occurred 20 h after the total gradient of the magnetic field of the entire region calculated from SDO/HMI data reached its maximum value. Analysis of the evolution of the microwave source that appeared before the X-flare in AR 12242 and comparison of its parameters with the parameters of other components of the AR microwave radiation showed that the new source can be classified as neutral line associated source (NLS), which were repeatedly detected by the RATAN-600 and other radio telescopes 1-3 days before the large flares.

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Applying an Automatic Image-Processing Method to Synoptic Observations

Cited by 32 publications

References 16 publications

Creation of Series of Properties of Individual Sunspots

Creation of Series of Properties of Individual Sunspots

Evolution of Solar Active Region 12673 by Ratan-600 and Sdo Data

Features of Microwave Radiation and Magnetographic Characteristics of Solar Active Region NOAA 12242 Before the X1.8 Flare on December 20, 2014

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