Negative magnetic buoyancy and formation of a sunspot belt
Magnetic buoyancy constrains the magnitude of toroidal field excited by the Ω-effect near the bottom of the solar convection zone (SCZ). Therefore, we examined two negative magnetic buoyancy effects: i) macroscopic turbulent diamagnetism (the γ-effect) and ii) magnetic advection caused by vertical i...
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| Опубліковано в: : | Кинематика и физика небесных тел |
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| Дата: | 2005 |
| Автор: | |
| Формат: | Стаття |
| Мова: | Англійська |
| Опубліковано: |
Головна астрономічна обсерваторія НАН України
2005
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| Онлайн доступ: | https://nasplib.isofts.kiev.ua/handle/123456789/79632 |
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| Назва журналу: | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| Цитувати: | Negative magnetic buoyancy and formation of a sunspot belt / V.N. Kryvodubskyj // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 155-158. — Бібліогр.: 18 назв. — англ. |
Репозитарії
Digital Library of Periodicals of National Academy of Sciences of Ukraine| _version_ | 1862741024794738688 |
|---|---|
| author | Kryvodubskyj, V.N. |
| author_facet | Kryvodubskyj, V.N. |
| citation_txt | Negative magnetic buoyancy and formation of a sunspot belt / V.N. Kryvodubskyj // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 155-158. — Бібліогр.: 18 назв. — англ. |
| collection | DSpace DC |
| container_title | Кинематика и физика небесных тел |
| description | Magnetic buoyancy constrains the magnitude of toroidal field excited by the Ω-effect near the bottom of the solar convection zone (SCZ). Therefore, we examined two negative magnetic buoyancy effects: i) macroscopic turbulent diamagnetism (the γ-effect) and ii) magnetic advection caused by vertical inhomogeneity of plasma density in the SCZ, which we called the ∇ρ-effect. The Sun’s rotation which yields the ∇ρ-effect with new properties was taken into account. The reconstruction of toroidal field was calculated as a result of the balance of mean-field magnetic buoyancy, turbulent diamagnetism and the rotationally modified ∇ρ-effect. It is shown that at high latitudes negative buoyancy effects block the magnetic fields in the deep layers of the SCZ, and this may be the most plausible reason why a deep-seated field here could not become as apparent at the solar surface as sunspots. However, in the region located near equator the ∇ρ-effect causes the upward magnetic advection. So, it can facilitate penetration of strong magnetic fields (about 3000–4000 G) to solar surface where they then arise in the “royal zone” as the sunspots
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| first_indexed | 2025-12-07T20:17:39Z |
| format | Article |
| fulltext | |
| id | nasplib_isofts_kiev_ua-123456789-79632 |
| institution | Digital Library of Periodicals of National Academy of Sciences of Ukraine |
| issn | 0233-7665 |
| language | English |
| last_indexed | 2025-12-07T20:17:39Z |
| publishDate | 2005 |
| publisher | Головна астрономічна обсерваторія НАН України |
| record_format | dspace |
| spelling | Kryvodubskyj, V.N. 2015-04-03T16:41:26Z 2015-04-03T16:41:26Z 2005 Negative magnetic buoyancy and formation of a sunspot belt / V.N. Kryvodubskyj // Кинематика и физика небесных тел. — 2005. — Т. 21, № 5-додаток. — С. 155-158. — Бібліогр.: 18 назв. — англ. 0233-7665 https://nasplib.isofts.kiev.ua/handle/123456789/79632 Magnetic buoyancy constrains the magnitude of toroidal field excited by the Ω-effect near the bottom of the solar convection zone (SCZ). Therefore, we examined two negative magnetic buoyancy effects: i) macroscopic turbulent diamagnetism (the γ-effect) and ii) magnetic advection caused by vertical inhomogeneity of plasma density in the SCZ, which we called the ∇ρ-effect. The Sun’s rotation which yields the ∇ρ-effect with new properties was taken into account. The reconstruction of toroidal field was calculated as a result of the balance of mean-field magnetic buoyancy, turbulent diamagnetism and the rotationally modified ∇ρ-effect. It is shown that at high latitudes negative buoyancy effects block the magnetic fields in the deep layers of the SCZ, and this may be the most plausible reason why a deep-seated field here could not become as apparent at the solar surface as sunspots. However, in the region located near equator the ∇ρ-effect causes the upward magnetic advection. So, it can facilitate penetration of strong magnetic fields (about 3000–4000 G) to solar surface where they then arise in the “royal zone” as the sunspots Author thanks L. L. Kitchatinov for a useful discussion en Головна астрономічна обсерваторія НАН України Кинематика и физика небесных тел MS2: Physics of Solar Atmosphere Negative magnetic buoyancy and formation of a sunspot belt Article published earlier |
| spellingShingle | Negative magnetic buoyancy and formation of a sunspot belt Kryvodubskyj, V.N. MS2: Physics of Solar Atmosphere |
| title | Negative magnetic buoyancy and formation of a sunspot belt |
| title_full | Negative magnetic buoyancy and formation of a sunspot belt |
| title_fullStr | Negative magnetic buoyancy and formation of a sunspot belt |
| title_full_unstemmed | Negative magnetic buoyancy and formation of a sunspot belt |
| title_short | Negative magnetic buoyancy and formation of a sunspot belt |
| title_sort | negative magnetic buoyancy and formation of a sunspot belt |
| topic | MS2: Physics of Solar Atmosphere |
| topic_facet | MS2: Physics of Solar Atmosphere |
| url | https://nasplib.isofts.kiev.ua/handle/123456789/79632 |
| work_keys_str_mv | AT kryvodubskyjvn negativemagneticbuoyancyandformationofasunspotbelt |