Distribution of low-power solar flares by brightness rise time

Aleksandr Borovik; Anton Zhdanov

doi:10.12737/stp-43201801

UDC 52

DISTRIBUTION OF LOW-POWER SOLAR FLARES BY BRIGHTNESS RISE TIME Distribution of low-power solar flares by brightness rise time

АА Аа

Published in Solar-Terrestrial Physics · Volume 4, Issue 3 · Pages 3–12 · Rubric: Results of current research

DOI: https://doi.org/10.12737/stp-43201801

Received: 28.09.2018 Accepted: 16.03.2026 Language of publication: ENG

Authors

Aleksandr Borovik

ORCID

Anton Zhdanov

ORCID

Aleksandr Borovik

Academic degree: candidate of physical and mathematical sciences

Institute of Solar Terrestrial Physics SB RAS Russian Federation · Irkutsk

ORCID

Anton Zhdanov

Institute of Solar Terrestrial Physics SB RAS Russian Federation · Irkutsk

ORCID

ABSTRACT

Using data from the international flare patrol for 1972–2010, we have formed an electronic database for more than 123 thousand solar flares. We determined the mean brightness rise time (flash phase) for flare area classes and importance. We show that the mean flash phase increased with increasing area class. For brightness classes this trend is less pronounced. We have found that flares with explosive phase and flares with one brilliant point have the shortest flash phases; two-ribbon flares and flares with several intensity maxima, the longest ones. We have separated 572 cases when the brightness rise time was more than 60 min; 80 % of such ultra-long flares have a shorter brightness decay time (main phase). We have established that low-power flares in terms of developmental features do not differ from large flares. Low-power solar flares, as well as large flares, can be followed by filament activation or disappearance, and can have an explosive phase and several intensity maxima. Two-ribbon flares, white-light flares, and flares covering sunspot umbra can also have low power.

KEYWORDS

solar activity, solar flares

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Geliy Zherebtsov

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Deputy Editor-in-Chief

Aleksandr Stepanov

stepanov@gaoran.ru

Deputy Editor-in-Chief

Alexander Potapov

potapov@iszf.irk.ru

Executive Secretary of Editorial Board

Natalia Polyushkina

npol@iszf.irk.ru

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Borovik A. V., Zhdanov A. A. Distribution of low-power solar flares by brightness rise time // Solar-Terrestrial Physics. 2018. no. 3. pp. 3-12. DOI: https://doi.org/10.12737/stp-43201801. (Date of access 23.09.2026).

MLA

Aleksandr Borovik, Zhdanov A. A.. "Distribution of low-power solar flares by brightness rise time." Solar-Terrestrial Physics 4.3 (2018): 3-12. DOI: https://doi.org/10.12737/stp-43201801.

APA

Borovik A. V., Zhdanov A. A. (2018). Distribution of low-power solar flares by brightness rise time. Solar-Terrestrial Physics, 4(3), 3-12. https://doi.org/10.12737/stp-43201801

Chicago

Aleksandr Borovik, Zhdanov A. A.. "Distribution of low-power solar flares by brightness rise time." Solar-Terrestrial Physics 4, no. 3 (2018): 3-12. https://doi.org/10.12737/stp-43201801.

WIKI

{{cite journal | author = Borovik A. V., Zhdanov A. A. | title = Distribution of low-power solar flares by brightness rise time | journal = Solar-Terrestrial Physics | year = 2018 | volume = 4 | issue = 3 | pages = 3-12 | doi = 10.12737/stp-43201801 }}

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DISTRIBUTION OF LOW-POWER SOLAR FLARES BY BRIGHTNESS RISE TIME Distribution of low-power solar flares by brightness rise time

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