The peculiarities of rotation of the solar polar regions
Abstract The sidereal rotation rate of the high-latitude solar regions is examined using long-lived photospheric polar faculae. The observations were carried out with the photoheliograph of Kislovodsk Mountain Station of the Pulkovo Observatory from 1982 to 1986. The following facts have been establ...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Solonsky, Yu. A. [verfasserIn] |
|---|
| Format: |
Artikel |
|---|---|
| Sprache: |
Englisch |
| Erschienen: |
1992 |
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| Schlagwörter: |
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| Anmerkung: |
© Kluwer Academic Publishers 1992 |
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| Übergeordnetes Werk: |
Enthalten in: Solar physics - Kluwer Academic Publishers, 1967, 139(1992), 2 vom: Juni, Seite 233-245 |
|---|---|
| Übergeordnetes Werk: |
volume:139 ; year:1992 ; number:2 ; month:06 ; pages:233-245 |
| Links: |
|---|
| DOI / URN: |
10.1007/BF00159150 |
|---|
| Katalog-ID: |
OLC2033571270 |
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| 520 | |a Abstract The sidereal rotation rate of the high-latitude solar regions is examined using long-lived photospheric polar faculae. The observations were carried out with the photoheliograph of Kislovodsk Mountain Station of the Pulkovo Observatory from 1982 to 1986. The following facts have been established: (a) There is a differential rotation of the polar faculae close to the maximum of solar activity, while the amount of latitude gradient of solar rotation decreases towards the sunspot minimum; (b) small differences of rotation in the northern and southern hemispheres of the Sun are observed; (c) some deviations of differential rotation curves constructed for each Carrington rotation from the mean curve of differential rotation are revealed. The total amplitude of the maximum positive and negative excesses is about 40–50 m $ s^{−1} $. The positive surplus velocities of solar rotation (the amplitude of which is about 20–25 m $ s^{−1} $) move in the form of a wave from heliographic latitudes ≈40° with a velocity of 1.6 m $ s^{−1} $. The latitude width of this flow is ΔB ≈ 15°. This wave of abnormally high velocity starts in the year of minimum solar activity and reaches the pole 11 years later. The picture is symmetrical relative to the equator. | ||
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10.1007/BF00159150 doi (DE-627)OLC2033571270 (DE-He213)BF00159150-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Solonsky, Yu. A. verfasserin aut The peculiarities of rotation of the solar polar regions 1992 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1992 Abstract The sidereal rotation rate of the high-latitude solar regions is examined using long-lived photospheric polar faculae. The observations were carried out with the photoheliograph of Kislovodsk Mountain Station of the Pulkovo Observatory from 1982 to 1986. The following facts have been established: (a) There is a differential rotation of the polar faculae close to the maximum of solar activity, while the amount of latitude gradient of solar rotation decreases towards the sunspot minimum; (b) small differences of rotation in the northern and southern hemispheres of the Sun are observed; (c) some deviations of differential rotation curves constructed for each Carrington rotation from the mean curve of differential rotation are revealed. The total amplitude of the maximum positive and negative excesses is about 40–50 m $ s^{−1} $. The positive surplus velocities of solar rotation (the amplitude of which is about 20–25 m $ s^{−1} $) move in the form of a wave from heliographic latitudes ≈40° with a velocity of 1.6 m $ s^{−1} $. The latitude width of this flow is ΔB ≈ 15°. This wave of abnormally high velocity starts in the year of minimum solar activity and reaches the pole 11 years later. The picture is symmetrical relative to the equator. Solar Activity Rotation Curve Differential Rotation Solar Rotation Carrington Rotation Makarova, V. V. aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 139(1992), 2 vom: Juni, Seite 233-245 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:139 year:1992 number:2 month:06 pages:233-245 https://doi.org/10.1007/BF00159150 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4306 AR 139 1992 2 06 233-245 |
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10.1007/BF00159150 doi (DE-627)OLC2033571270 (DE-He213)BF00159150-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Solonsky, Yu. A. verfasserin aut The peculiarities of rotation of the solar polar regions 1992 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1992 Abstract The sidereal rotation rate of the high-latitude solar regions is examined using long-lived photospheric polar faculae. The observations were carried out with the photoheliograph of Kislovodsk Mountain Station of the Pulkovo Observatory from 1982 to 1986. The following facts have been established: (a) There is a differential rotation of the polar faculae close to the maximum of solar activity, while the amount of latitude gradient of solar rotation decreases towards the sunspot minimum; (b) small differences of rotation in the northern and southern hemispheres of the Sun are observed; (c) some deviations of differential rotation curves constructed for each Carrington rotation from the mean curve of differential rotation are revealed. The total amplitude of the maximum positive and negative excesses is about 40–50 m $ s^{−1} $. The positive surplus velocities of solar rotation (the amplitude of which is about 20–25 m $ s^{−1} $) move in the form of a wave from heliographic latitudes ≈40° with a velocity of 1.6 m $ s^{−1} $. The latitude width of this flow is ΔB ≈ 15°. This wave of abnormally high velocity starts in the year of minimum solar activity and reaches the pole 11 years later. The picture is symmetrical relative to the equator. Solar Activity Rotation Curve Differential Rotation Solar Rotation Carrington Rotation Makarova, V. V. aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 139(1992), 2 vom: Juni, Seite 233-245 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:139 year:1992 number:2 month:06 pages:233-245 https://doi.org/10.1007/BF00159150 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4306 AR 139 1992 2 06 233-245 |
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10.1007/BF00159150 doi (DE-627)OLC2033571270 (DE-He213)BF00159150-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Solonsky, Yu. A. verfasserin aut The peculiarities of rotation of the solar polar regions 1992 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1992 Abstract The sidereal rotation rate of the high-latitude solar regions is examined using long-lived photospheric polar faculae. The observations were carried out with the photoheliograph of Kislovodsk Mountain Station of the Pulkovo Observatory from 1982 to 1986. The following facts have been established: (a) There is a differential rotation of the polar faculae close to the maximum of solar activity, while the amount of latitude gradient of solar rotation decreases towards the sunspot minimum; (b) small differences of rotation in the northern and southern hemispheres of the Sun are observed; (c) some deviations of differential rotation curves constructed for each Carrington rotation from the mean curve of differential rotation are revealed. The total amplitude of the maximum positive and negative excesses is about 40–50 m $ s^{−1} $. The positive surplus velocities of solar rotation (the amplitude of which is about 20–25 m $ s^{−1} $) move in the form of a wave from heliographic latitudes ≈40° with a velocity of 1.6 m $ s^{−1} $. The latitude width of this flow is ΔB ≈ 15°. This wave of abnormally high velocity starts in the year of minimum solar activity and reaches the pole 11 years later. The picture is symmetrical relative to the equator. Solar Activity Rotation Curve Differential Rotation Solar Rotation Carrington Rotation Makarova, V. V. aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 139(1992), 2 vom: Juni, Seite 233-245 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:139 year:1992 number:2 month:06 pages:233-245 https://doi.org/10.1007/BF00159150 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4306 AR 139 1992 2 06 233-245 |
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10.1007/BF00159150 doi (DE-627)OLC2033571270 (DE-He213)BF00159150-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Solonsky, Yu. A. verfasserin aut The peculiarities of rotation of the solar polar regions 1992 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1992 Abstract The sidereal rotation rate of the high-latitude solar regions is examined using long-lived photospheric polar faculae. The observations were carried out with the photoheliograph of Kislovodsk Mountain Station of the Pulkovo Observatory from 1982 to 1986. The following facts have been established: (a) There is a differential rotation of the polar faculae close to the maximum of solar activity, while the amount of latitude gradient of solar rotation decreases towards the sunspot minimum; (b) small differences of rotation in the northern and southern hemispheres of the Sun are observed; (c) some deviations of differential rotation curves constructed for each Carrington rotation from the mean curve of differential rotation are revealed. The total amplitude of the maximum positive and negative excesses is about 40–50 m $ s^{−1} $. The positive surplus velocities of solar rotation (the amplitude of which is about 20–25 m $ s^{−1} $) move in the form of a wave from heliographic latitudes ≈40° with a velocity of 1.6 m $ s^{−1} $. The latitude width of this flow is ΔB ≈ 15°. This wave of abnormally high velocity starts in the year of minimum solar activity and reaches the pole 11 years later. The picture is symmetrical relative to the equator. Solar Activity Rotation Curve Differential Rotation Solar Rotation Carrington Rotation Makarova, V. V. aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 139(1992), 2 vom: Juni, Seite 233-245 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:139 year:1992 number:2 month:06 pages:233-245 https://doi.org/10.1007/BF00159150 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4306 AR 139 1992 2 06 233-245 |
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10.1007/BF00159150 doi (DE-627)OLC2033571270 (DE-He213)BF00159150-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Solonsky, Yu. A. verfasserin aut The peculiarities of rotation of the solar polar regions 1992 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1992 Abstract The sidereal rotation rate of the high-latitude solar regions is examined using long-lived photospheric polar faculae. The observations were carried out with the photoheliograph of Kislovodsk Mountain Station of the Pulkovo Observatory from 1982 to 1986. The following facts have been established: (a) There is a differential rotation of the polar faculae close to the maximum of solar activity, while the amount of latitude gradient of solar rotation decreases towards the sunspot minimum; (b) small differences of rotation in the northern and southern hemispheres of the Sun are observed; (c) some deviations of differential rotation curves constructed for each Carrington rotation from the mean curve of differential rotation are revealed. The total amplitude of the maximum positive and negative excesses is about 40–50 m $ s^{−1} $. The positive surplus velocities of solar rotation (the amplitude of which is about 20–25 m $ s^{−1} $) move in the form of a wave from heliographic latitudes ≈40° with a velocity of 1.6 m $ s^{−1} $. The latitude width of this flow is ΔB ≈ 15°. This wave of abnormally high velocity starts in the year of minimum solar activity and reaches the pole 11 years later. The picture is symmetrical relative to the equator. Solar Activity Rotation Curve Differential Rotation Solar Rotation Carrington Rotation Makarova, V. V. aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 139(1992), 2 vom: Juni, Seite 233-245 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:139 year:1992 number:2 month:06 pages:233-245 https://doi.org/10.1007/BF00159150 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4306 AR 139 1992 2 06 233-245 |
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Solonsky, Yu. A. Makarova, V. V. |
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Solonsky, Yu. A. |
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the peculiarities of rotation of the solar polar regions |
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The peculiarities of rotation of the solar polar regions |
| abstract |
Abstract The sidereal rotation rate of the high-latitude solar regions is examined using long-lived photospheric polar faculae. The observations were carried out with the photoheliograph of Kislovodsk Mountain Station of the Pulkovo Observatory from 1982 to 1986. The following facts have been established: (a) There is a differential rotation of the polar faculae close to the maximum of solar activity, while the amount of latitude gradient of solar rotation decreases towards the sunspot minimum; (b) small differences of rotation in the northern and southern hemispheres of the Sun are observed; (c) some deviations of differential rotation curves constructed for each Carrington rotation from the mean curve of differential rotation are revealed. The total amplitude of the maximum positive and negative excesses is about 40–50 m $ s^{−1} $. The positive surplus velocities of solar rotation (the amplitude of which is about 20–25 m $ s^{−1} $) move in the form of a wave from heliographic latitudes ≈40° with a velocity of 1.6 m $ s^{−1} $. The latitude width of this flow is ΔB ≈ 15°. This wave of abnormally high velocity starts in the year of minimum solar activity and reaches the pole 11 years later. The picture is symmetrical relative to the equator. © Kluwer Academic Publishers 1992 |
| abstractGer |
Abstract The sidereal rotation rate of the high-latitude solar regions is examined using long-lived photospheric polar faculae. The observations were carried out with the photoheliograph of Kislovodsk Mountain Station of the Pulkovo Observatory from 1982 to 1986. The following facts have been established: (a) There is a differential rotation of the polar faculae close to the maximum of solar activity, while the amount of latitude gradient of solar rotation decreases towards the sunspot minimum; (b) small differences of rotation in the northern and southern hemispheres of the Sun are observed; (c) some deviations of differential rotation curves constructed for each Carrington rotation from the mean curve of differential rotation are revealed. The total amplitude of the maximum positive and negative excesses is about 40–50 m $ s^{−1} $. The positive surplus velocities of solar rotation (the amplitude of which is about 20–25 m $ s^{−1} $) move in the form of a wave from heliographic latitudes ≈40° with a velocity of 1.6 m $ s^{−1} $. The latitude width of this flow is ΔB ≈ 15°. This wave of abnormally high velocity starts in the year of minimum solar activity and reaches the pole 11 years later. The picture is symmetrical relative to the equator. © Kluwer Academic Publishers 1992 |
| abstract_unstemmed |
Abstract The sidereal rotation rate of the high-latitude solar regions is examined using long-lived photospheric polar faculae. The observations were carried out with the photoheliograph of Kislovodsk Mountain Station of the Pulkovo Observatory from 1982 to 1986. The following facts have been established: (a) There is a differential rotation of the polar faculae close to the maximum of solar activity, while the amount of latitude gradient of solar rotation decreases towards the sunspot minimum; (b) small differences of rotation in the northern and southern hemispheres of the Sun are observed; (c) some deviations of differential rotation curves constructed for each Carrington rotation from the mean curve of differential rotation are revealed. The total amplitude of the maximum positive and negative excesses is about 40–50 m $ s^{−1} $. The positive surplus velocities of solar rotation (the amplitude of which is about 20–25 m $ s^{−1} $) move in the form of a wave from heliographic latitudes ≈40° with a velocity of 1.6 m $ s^{−1} $. The latitude width of this flow is ΔB ≈ 15°. This wave of abnormally high velocity starts in the year of minimum solar activity and reaches the pole 11 years later. The picture is symmetrical relative to the equator. © Kluwer Academic Publishers 1992 |
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The peculiarities of rotation of the solar polar regions |
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