Fine structure of convective motions in the solar photosphere
The granulation brightnesses and convective velocities in the solar photosphere between the levels of formation of the continuum radiation and the temperature minimum are examined. The properties of the brightness and velocity are analysed in a sixteen-column model. Four sorts of motions are most ty...
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| Published in: | Кинематика и физика небесных тел |
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| Date: | 2005 |
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| Format: | Article |
| Language: | English |
| Published: |
Головна астрономічна обсерваторія НАН України
2005
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| Online Access: | https://nasplib.isofts.kiev.ua/handle/123456789/79619 |
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| Journal Title: | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| Cite this: | Fine structure of convective motions in the solar photosphere / R.I. Kostik // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 134-137. — Бібліогр.: 2 назв. — англ. |
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Digital Library of Periodicals of National Academy of Sciences of Ukraine| id |
nasplib_isofts_kiev_ua-123456789-79619 |
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Kostik, R.I. 2015-04-03T15:51:44Z 2015-04-03T15:51:44Z 2005 Fine structure of convective motions in the solar photosphere / R.I. Kostik // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 134-137. — Бібліогр.: 2 назв. — англ. 0233-7665 https://nasplib.isofts.kiev.ua/handle/123456789/79619 The granulation brightnesses and convective velocities in the solar photosphere between the levels of formation of the continuum radiation and the temperature minimum are examined. The properties of the brightness and velocity are analysed in a sixteen-column model. Four sorts of motions are most typical and efficient. In the first two, only the sign of the relative contrast of the material changes, which occurs, on the average, at a height of 270 km. In the last two motions, both the sign of the contrast and the direction of the motions are reversed near ~350 km. The convective motions maintain their column structure throughout the photosphere, right to the temperature minimum. The author are grateful to N. Shchukina and E. Khomenko for providing me with the observational data. This work was partially supported by the Fundamental Research State Fund of the Ministry of Ukraine for Education and Science (project No. 02.07/00044) and INTAS (project 00–00084). en Головна астрономічна обсерваторія НАН України Кинематика и физика небесных тел MS2: Physics of Solar Atmosphere Fine structure of convective motions in the solar photosphere Article published earlier |
| institution |
Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| collection |
DSpace DC |
| title |
Fine structure of convective motions in the solar photosphere |
| spellingShingle |
Fine structure of convective motions in the solar photosphere Kostik, R.I. MS2: Physics of Solar Atmosphere |
| title_short |
Fine structure of convective motions in the solar photosphere |
| title_full |
Fine structure of convective motions in the solar photosphere |
| title_fullStr |
Fine structure of convective motions in the solar photosphere |
| title_full_unstemmed |
Fine structure of convective motions in the solar photosphere |
| title_sort |
fine structure of convective motions in the solar photosphere |
| author |
Kostik, R.I. |
| author_facet |
Kostik, R.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 |
The granulation brightnesses and convective velocities in the solar photosphere between the levels of formation of the continuum radiation and the temperature minimum are examined. The properties of the brightness and velocity are analysed in a sixteen-column model. Four sorts of motions are most typical and efficient. In the first two, only the sign of the relative contrast of the material changes, which occurs, on the average, at a height of 270 km. In the last two motions, both the sign of the contrast and the direction of the motions are reversed near ~350 km. The convective motions maintain their column structure throughout the photosphere, right to the temperature minimum.
|
| issn |
0233-7665 |
| url |
https://nasplib.isofts.kiev.ua/handle/123456789/79619 |
| citation_txt |
Fine structure of convective motions in the solar photosphere / R.I. Kostik // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 134-137. — Бібліогр.: 2 назв. — англ. |
| work_keys_str_mv |
AT kostikri finestructureofconvectivemotionsinthesolarphotosphere |
| first_indexed |
2025-12-07T18:46:37Z |
| last_indexed |
2025-12-07T18:46:37Z |
| _version_ |
1850876307532939264 |