Distribution of low-power solar flares by brightness rise time-Reference-Cited by-同舟云学术

Distribution of low-power solar flares by brightness rise time

Published:2018-09-28 Issue:3 Volume:4 Page:3-12
ISSN:2500-0535
Container-title:Solar-Terrestrial Physics
language:en
Short-container-title:

Author:

Боровик Александр¹,Borovik Aleksandr²,Жданов Антон¹,Zhdanov Anton²

Affiliation:

1. Институт солнечно-земной физики СО РАН

2. Institute of Solar Terrestrial Physics SB RAS

Abstract

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.

Publisher

Infra-M Academic Publishing House

Subject

Space and Planetary Science,Atmospheric Science,Geophysics

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