Variations of the energy spectra of solar X-ray flares: interconnection with the photospheric, chromospheric, and magnetic activity of the Sun (1972−2001)

Variations of the energy spectra of solar X-ray flares: interconnection with the photospheric, chromospheric, and magnetic activity of the Sun (1972−2001)

The problem of flare energy distribution of the Sun is strongly related to the power-law energy spectra of flares on the UV Ceti-type stars. In a preliminary study (1972–1993), the X-ray flare integral energy spectrum (IES) was represented by a unique power law of N ~ E−b with index b = 0.76. Later...

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Бібліографічні деталі
Дата:2005
Автор: Kasinskii, V.
Формат: Стаття
Мова:English
Опубліковано: Головна астрономічна обсерваторія НАН України 2005
Назва видання:Кинематика и физика небесных тел
Теми:
MS2: Physics of Solar Atmosphere
Онлайн доступ:http://dspace.nbuv.gov.ua/handle/123456789/79614
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Назва журналу:Digital Library of Periodicals of National Academy of Sciences of Ukraine
Цитувати:Variations of the energy spectra of solar X-ray flares: interconnection with the photospheric, chromospheric, and magnetic activity of the Sun (1972−2001) / V. Kasinskii // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 105-109. — Бібліогр.: 5 назв. — англ.

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Digital Library of Periodicals of National Academy of Sciences of Ukraine
id irk-123456789-79614
record_format dspace
spelling irk-123456789-796142015-04-04T03:01:51Z Variations of the energy spectra of solar X-ray flares: interconnection with the photospheric, chromospheric, and magnetic activity of the Sun (1972−2001) Kasinskii, V. MS2: Physics of Solar Atmosphere The problem of flare energy distribution of the Sun is strongly related to the power-law energy spectra of flares on the UV Ceti-type stars. In a preliminary study (1972–1993), the X-ray flare integral energy spectrum (IES) was represented by a unique power law of N ~ E−b with index b = 0.76. Later it was shown that the exponent index b varies with the cycle phase, that is with the Wolf number. The purpose of this paper is to investigate the temporal variations in the power-law spectrum of soft X-ray flares over the three solar cycles (1972–2001). A more extensive statistic (56 000 flares) allows us to revise earlier results and to derive new ones. Not only b-index undergoes variations associated with a 11-year cycle but the limiting energy of flares (log Em) as well. The three-cycle-averaged b is 0.666, with variations in the range 0.50 < b < 0.80. The results may be useful for study of flare activity on red dwarf stars. 2005 Article Variations of the energy spectra of solar X-ray flares: interconnection with the photospheric, chromospheric, and magnetic activity of the Sun (1972−2001) / V. Kasinskii // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 105-109. — Бібліогр.: 5 назв. — англ. 0233-7665 http://dspace.nbuv.gov.ua/handle/123456789/79614 en Кинематика и физика небесных тел Головна астрономічна обсерваторія НАН України
institution Digital Library of Periodicals of National Academy of Sciences of Ukraine
collection DSpace DC
language English
topic MS2: Physics of Solar Atmosphere
MS2: Physics of Solar Atmosphere
spellingShingle MS2: Physics of Solar Atmosphere
MS2: Physics of Solar Atmosphere
Kasinskii, V.
Variations of the energy spectra of solar X-ray flares: interconnection with the photospheric, chromospheric, and magnetic activity of the Sun (1972−2001)
Кинематика и физика небесных тел
description The problem of flare energy distribution of the Sun is strongly related to the power-law energy spectra of flares on the UV Ceti-type stars. In a preliminary study (1972–1993), the X-ray flare integral energy spectrum (IES) was represented by a unique power law of N ~ E−b with index b = 0.76. Later it was shown that the exponent index b varies with the cycle phase, that is with the Wolf number. The purpose of this paper is to investigate the temporal variations in the power-law spectrum of soft X-ray flares over the three solar cycles (1972–2001). A more extensive statistic (56 000 flares) allows us to revise earlier results and to derive new ones. Not only b-index undergoes variations associated with a 11-year cycle but the limiting energy of flares (log Em) as well. The three-cycle-averaged b is 0.666, with variations in the range 0.50 < b < 0.80. The results may be useful for study of flare activity on red dwarf stars.
format Article
author Kasinskii, V.
author_facet Kasinskii, V.
author_sort Kasinskii, V.
title Variations of the energy spectra of solar X-ray flares: interconnection with the photospheric, chromospheric, and magnetic activity of the Sun (1972−2001)
title_short Variations of the energy spectra of solar X-ray flares: interconnection with the photospheric, chromospheric, and magnetic activity of the Sun (1972−2001)
title_full Variations of the energy spectra of solar X-ray flares: interconnection with the photospheric, chromospheric, and magnetic activity of the Sun (1972−2001)
title_fullStr Variations of the energy spectra of solar X-ray flares: interconnection with the photospheric, chromospheric, and magnetic activity of the Sun (1972−2001)
title_full_unstemmed Variations of the energy spectra of solar X-ray flares: interconnection with the photospheric, chromospheric, and magnetic activity of the Sun (1972−2001)
title_sort variations of the energy spectra of solar x-ray flares: interconnection with the photospheric, chromospheric, and magnetic activity of the sun (1972−2001)
publisher Головна астрономічна обсерваторія НАН України
publishDate 2005
topic_facet MS2: Physics of Solar Atmosphere
url http://dspace.nbuv.gov.ua/handle/123456789/79614
citation_txt Variations of the energy spectra of solar X-ray flares: interconnection with the photospheric, chromospheric, and magnetic activity of the Sun (1972−2001) / V. Kasinskii // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 105-109. — Бібліогр.: 5 назв. — англ.
series Кинематика и физика небесных тел
work_keys_str_mv AT kasinskiiv variationsoftheenergyspectraofsolarxrayflaresinterconnectionwiththephotosphericchromosphericandmagneticactivityofthesun19722001
first_indexed 2023-10-18T19:19:06Z
last_indexed 2023-10-18T19:19:06Z
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