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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| Published in: | Кинематика и физика небесных тел |
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| Date: | 2005 |
| Main Authors: | , |
| Format: | Article |
| Language: | English |
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Головна астрономічна обсерваторія НАН України
2005
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| Online Access: | https://nasplib.isofts.kiev.ua/handle/123456789/79629 |
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| Cite this: | 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. |
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Lozitsky, V.G. Lozitska, N.I. 2015-04-03T16:33:57Z 2015-04-03T16:33:57Z 2005 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 https://nasplib.isofts.kiev.ua/handle/123456789/79629 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. en Головна астрономічна обсерваторія НАН України Кинематика и физика небесных тел MS2: Physics of Solar Atmosphere Line profiles and magnetic fields in the exclusively powerful solar flare of October 28, 2003: preliminary results Article published earlier |
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Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| collection |
DSpace DC |
| title |
Line profiles and magnetic fields in the exclusively powerful solar flare of October 28, 2003: preliminary results |
| spellingShingle |
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 |
| 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 |
| author |
Lozitsky, V.G. Lozitska, N.I. |
| author_facet |
Lozitsky, V.G. Lozitska, N.I. |
| topic |
MS2: Physics of Solar Atmosphere |
| topic_facet |
MS2: Physics of Solar Atmosphere |
| publishDate |
2005 |
| language |
English |
| container_title |
Кинематика и физика небесных тел |
| publisher |
Головна астрономічна обсерваторія НАН України |
| format |
Article |
| 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.
|
| issn |
0233-7665 |
| url |
https://nasplib.isofts.kiev.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. |
| work_keys_str_mv |
AT lozitskyvg lineprofilesandmagneticfieldsintheexclusivelypowerfulsolarflareofoctober282003preliminaryresults AT lozitskani lineprofilesandmagneticfieldsintheexclusivelypowerfulsolarflareofoctober282003preliminaryresults |
| first_indexed |
2025-12-07T20:10:40Z |
| last_indexed |
2025-12-07T20:10:40Z |
| _version_ |
1850881596009218048 |