Line profiles and magnetic fields in the exclusively powerful solar flare of October 28, 2003: preliminary results
We investigate the X17.2/4B solar flare of October 28, 2003 which has been occupying the third place among X-ray fluxes since 1975. The echelle Zeeman spectrograms obtained at the Kyiv University Astronomical Observatory allow us to conclude the following: a) observed flare emission in some magnetos...
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| Дата: | 2005 |
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| Автори: | , |
| Формат: | Стаття |
| Мова: | English |
| Опубліковано: |
Головна астрономічна обсерваторія НАН України
2005
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| Назва видання: | Кинематика и физика небесных тел |
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| Онлайн доступ: | http://dspace.nbuv.gov.ua/handle/123456789/79629 |
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| Назва журналу: | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| Цитувати: | Line profiles and magnetic fields in the exclusively powerful solar flare of October 28, 2003: preliminary results / V.G. Lozitsky, N.I. Lozitska // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 148-150. — Бібліогр.: 7 назв. — англ. |
Репозитарії
Digital Library of Periodicals of National Academy of Sciences of Ukraine| id |
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irk-123456789-796292015-04-04T03:01:59Z Line profiles and magnetic fields in the exclusively powerful solar flare of October 28, 2003: preliminary results Lozitsky, V.G. Lozitska, N.I. MS2: Physics of Solar Atmosphere We investigate the X17.2/4B solar flare of October 28, 2003 which has been occupying the third place among X-ray fluxes since 1975. The echelle Zeeman spectrograms obtained at the Kyiv University Astronomical Observatory allow us to conclude the following: a) observed flare emission in some magnetosensitive metallic lines can produce a false magnetographic signal of opposite polarity in case of Babcock’s or filter magnetograph, b) considerable both horizontal and vertical magnetic field inhomogeneity existed in the flare. The longitudinal mean magnetic field strength B|| was maximal at chromospheric level, which follows from a comparison of data in the Fe I λ 630.25 nm, He I D3, NaI D1 and D2 lines. In particular, the line ratios B||(D2)/B||(630.25) ≈ 3.2 and B||(D3)/B||(630.25) ≈ 2.0 were derived. 2005 Article Line profiles and magnetic fields in the exclusively powerful solar flare of October 28, 2003: preliminary results / V.G. Lozitsky, N.I. Lozitska // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 148-150. — Бібліогр.: 7 назв. — англ. 0233-7665 http://dspace.nbuv.gov.ua/handle/123456789/79629 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 Lozitsky, V.G. Lozitska, N.I. Line profiles and magnetic fields in the exclusively powerful solar flare of October 28, 2003: preliminary results Кинематика и физика небесных тел |
| description |
We investigate the X17.2/4B solar flare of October 28, 2003 which has been occupying the third place among X-ray fluxes since 1975. The echelle Zeeman spectrograms obtained at the Kyiv University Astronomical Observatory allow us to conclude the following: a) observed flare emission in some magnetosensitive metallic lines can produce a false magnetographic signal of opposite polarity in case of Babcock’s or filter magnetograph, b) considerable both horizontal and vertical magnetic field inhomogeneity existed in the flare. The longitudinal mean magnetic field strength B|| was maximal at chromospheric level, which follows from a comparison of data in the Fe I λ 630.25 nm, He I D3, NaI D1 and D2 lines. In particular, the line ratios B||(D2)/B||(630.25) ≈ 3.2 and B||(D3)/B||(630.25) ≈ 2.0 were derived. |
| format |
Article |
| author |
Lozitsky, V.G. Lozitska, N.I. |
| author_facet |
Lozitsky, V.G. Lozitska, N.I. |
| author_sort |
Lozitsky, V.G. |
| title |
Line profiles and magnetic fields in the exclusively powerful solar flare of October 28, 2003: preliminary results |
| title_short |
Line profiles and magnetic fields in the exclusively powerful solar flare of October 28, 2003: preliminary results |
| title_full |
Line profiles and magnetic fields in the exclusively powerful solar flare of October 28, 2003: preliminary results |
| title_fullStr |
Line profiles and magnetic fields in the exclusively powerful solar flare of October 28, 2003: preliminary results |
| title_full_unstemmed |
Line profiles and magnetic fields in the exclusively powerful solar flare of October 28, 2003: preliminary results |
| title_sort |
line profiles and magnetic fields in the exclusively powerful solar flare of october 28, 2003: preliminary results |
| publisher |
Головна астрономічна обсерваторія НАН України |
| publishDate |
2005 |
| topic_facet |
MS2: Physics of Solar Atmosphere |
| url |
http://dspace.nbuv.gov.ua/handle/123456789/79629 |
| citation_txt |
Line profiles and magnetic fields in the exclusively powerful solar flare of October 28, 2003: preliminary results / V.G. Lozitsky, N.I. Lozitska // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 148-150. — Бібліогр.: 7 назв. — англ. |
| series |
Кинематика и физика небесных тел |
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AT lozitskyvg lineprofilesandmagneticfieldsintheexclusivelypowerfulsolarflareofoctober282003preliminaryresults AT lozitskani lineprofilesandmagneticfieldsintheexclusivelypowerfulsolarflareofoctober282003preliminaryresults |
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2023-10-18T19:19:08Z |
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2023-10-18T19:19:08Z |
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