Analytical Model of an Asymmetric Sunspot with a Steady Plasma Flow in its Penumbra
Abstract A new exact analytical solution to the stationary problem of ideal magnetohydrodynamics is derived for an unipolar asymmetric sunspot immersed in a realistic solar atmosphere. The radial and vertical profiles of pressure, plasma density, and temperature in the visible layers of the sunspot...
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Gespeichert in:
| Autor*in: |
Solov’ev, A. A. [verfasserIn] |
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| Format: |
Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2016 |
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| Schlagwörter: |
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| Anmerkung: |
© Springer Science+Business Media Dordrecht 2016 |
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| Übergeordnetes Werk: |
Enthalten in: Solar physics - Springer Netherlands, 1967, 291(2016), 6 vom: 28. Juni, Seite 1647-1663 |
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| Übergeordnetes Werk: |
volume:291 ; year:2016 ; number:6 ; day:28 ; month:06 ; pages:1647-1663 |
| Links: |
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| DOI / URN: |
10.1007/s11207-016-0922-1 |
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OLC2033620611 |
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| 520 | |a Abstract A new exact analytical solution to the stationary problem of ideal magnetohydrodynamics is derived for an unipolar asymmetric sunspot immersed in a realistic solar atmosphere. The radial and vertical profiles of pressure, plasma density, and temperature in the visible layers of the sunspot are calculated. The reduction in plasma density in the magnetic funnel of the sunspot, corresponding to the Wilson depression, is also obtained. The magnetic structure of the sunspot is given analytically in a realistic way: a part of the magnetic flux of the sunspot approaches the surrounding photosphere at the outer edge of the penumbra. The magnetic field of the sunspot is not assumed to be axially symmetric. For the first time, the angular dependence of the physical variables in this model allows us to simulate not only a deviation from the circular shape of the sunspot, but also a fine filamentary structure of the sunspot penumbra. The Alfvén Mach number (the ratio of the plasma speed to the Alfvén speed) is zero at the center of the sunspot and rises slowly toward the periphery of the sunspot; this corresponds to the structure of the Evershed flow in the penumbra. The Evershed flow in our model is mainly concentrated in dark penumbral filaments, as is observed. | ||
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10.1007/s11207-016-0922-1 doi (DE-627)OLC2033620611 (DE-He213)s11207-016-0922-1-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Solov’ev, A. A. verfasserin aut Analytical Model of an Asymmetric Sunspot with a Steady Plasma Flow in its Penumbra 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2016 Abstract A new exact analytical solution to the stationary problem of ideal magnetohydrodynamics is derived for an unipolar asymmetric sunspot immersed in a realistic solar atmosphere. The radial and vertical profiles of pressure, plasma density, and temperature in the visible layers of the sunspot are calculated. The reduction in plasma density in the magnetic funnel of the sunspot, corresponding to the Wilson depression, is also obtained. The magnetic structure of the sunspot is given analytically in a realistic way: a part of the magnetic flux of the sunspot approaches the surrounding photosphere at the outer edge of the penumbra. The magnetic field of the sunspot is not assumed to be axially symmetric. For the first time, the angular dependence of the physical variables in this model allows us to simulate not only a deviation from the circular shape of the sunspot, but also a fine filamentary structure of the sunspot penumbra. The Alfvén Mach number (the ratio of the plasma speed to the Alfvén speed) is zero at the center of the sunspot and rises slowly toward the periphery of the sunspot; this corresponds to the structure of the Evershed flow in the penumbra. The Evershed flow in our model is mainly concentrated in dark penumbral filaments, as is observed. Sun Sunspots Magnetic field Model Umbra Penumbra Kirichek, E. A. aut Enthalten in Solar physics Springer Netherlands, 1967 291(2016), 6 vom: 28. Juni, Seite 1647-1663 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:291 year:2016 number:6 day:28 month:06 pages:1647-1663 https://doi.org/10.1007/s11207-016-0922-1 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_47 GBV_ILN_70 AR 291 2016 6 28 06 1647-1663 |
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10.1007/s11207-016-0922-1 doi (DE-627)OLC2033620611 (DE-He213)s11207-016-0922-1-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Solov’ev, A. A. verfasserin aut Analytical Model of an Asymmetric Sunspot with a Steady Plasma Flow in its Penumbra 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2016 Abstract A new exact analytical solution to the stationary problem of ideal magnetohydrodynamics is derived for an unipolar asymmetric sunspot immersed in a realistic solar atmosphere. The radial and vertical profiles of pressure, plasma density, and temperature in the visible layers of the sunspot are calculated. The reduction in plasma density in the magnetic funnel of the sunspot, corresponding to the Wilson depression, is also obtained. The magnetic structure of the sunspot is given analytically in a realistic way: a part of the magnetic flux of the sunspot approaches the surrounding photosphere at the outer edge of the penumbra. The magnetic field of the sunspot is not assumed to be axially symmetric. For the first time, the angular dependence of the physical variables in this model allows us to simulate not only a deviation from the circular shape of the sunspot, but also a fine filamentary structure of the sunspot penumbra. The Alfvén Mach number (the ratio of the plasma speed to the Alfvén speed) is zero at the center of the sunspot and rises slowly toward the periphery of the sunspot; this corresponds to the structure of the Evershed flow in the penumbra. The Evershed flow in our model is mainly concentrated in dark penumbral filaments, as is observed. Sun Sunspots Magnetic field Model Umbra Penumbra Kirichek, E. A. aut Enthalten in Solar physics Springer Netherlands, 1967 291(2016), 6 vom: 28. Juni, Seite 1647-1663 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:291 year:2016 number:6 day:28 month:06 pages:1647-1663 https://doi.org/10.1007/s11207-016-0922-1 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_47 GBV_ILN_70 AR 291 2016 6 28 06 1647-1663 |
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10.1007/s11207-016-0922-1 doi (DE-627)OLC2033620611 (DE-He213)s11207-016-0922-1-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Solov’ev, A. A. verfasserin aut Analytical Model of an Asymmetric Sunspot with a Steady Plasma Flow in its Penumbra 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2016 Abstract A new exact analytical solution to the stationary problem of ideal magnetohydrodynamics is derived for an unipolar asymmetric sunspot immersed in a realistic solar atmosphere. The radial and vertical profiles of pressure, plasma density, and temperature in the visible layers of the sunspot are calculated. The reduction in plasma density in the magnetic funnel of the sunspot, corresponding to the Wilson depression, is also obtained. The magnetic structure of the sunspot is given analytically in a realistic way: a part of the magnetic flux of the sunspot approaches the surrounding photosphere at the outer edge of the penumbra. The magnetic field of the sunspot is not assumed to be axially symmetric. For the first time, the angular dependence of the physical variables in this model allows us to simulate not only a deviation from the circular shape of the sunspot, but also a fine filamentary structure of the sunspot penumbra. The Alfvén Mach number (the ratio of the plasma speed to the Alfvén speed) is zero at the center of the sunspot and rises slowly toward the periphery of the sunspot; this corresponds to the structure of the Evershed flow in the penumbra. The Evershed flow in our model is mainly concentrated in dark penumbral filaments, as is observed. Sun Sunspots Magnetic field Model Umbra Penumbra Kirichek, E. A. aut Enthalten in Solar physics Springer Netherlands, 1967 291(2016), 6 vom: 28. Juni, Seite 1647-1663 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:291 year:2016 number:6 day:28 month:06 pages:1647-1663 https://doi.org/10.1007/s11207-016-0922-1 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_47 GBV_ILN_70 AR 291 2016 6 28 06 1647-1663 |
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10.1007/s11207-016-0922-1 doi (DE-627)OLC2033620611 (DE-He213)s11207-016-0922-1-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Solov’ev, A. A. verfasserin aut Analytical Model of an Asymmetric Sunspot with a Steady Plasma Flow in its Penumbra 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2016 Abstract A new exact analytical solution to the stationary problem of ideal magnetohydrodynamics is derived for an unipolar asymmetric sunspot immersed in a realistic solar atmosphere. The radial and vertical profiles of pressure, plasma density, and temperature in the visible layers of the sunspot are calculated. The reduction in plasma density in the magnetic funnel of the sunspot, corresponding to the Wilson depression, is also obtained. The magnetic structure of the sunspot is given analytically in a realistic way: a part of the magnetic flux of the sunspot approaches the surrounding photosphere at the outer edge of the penumbra. The magnetic field of the sunspot is not assumed to be axially symmetric. For the first time, the angular dependence of the physical variables in this model allows us to simulate not only a deviation from the circular shape of the sunspot, but also a fine filamentary structure of the sunspot penumbra. The Alfvén Mach number (the ratio of the plasma speed to the Alfvén speed) is zero at the center of the sunspot and rises slowly toward the periphery of the sunspot; this corresponds to the structure of the Evershed flow in the penumbra. The Evershed flow in our model is mainly concentrated in dark penumbral filaments, as is observed. Sun Sunspots Magnetic field Model Umbra Penumbra Kirichek, E. A. aut Enthalten in Solar physics Springer Netherlands, 1967 291(2016), 6 vom: 28. Juni, Seite 1647-1663 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:291 year:2016 number:6 day:28 month:06 pages:1647-1663 https://doi.org/10.1007/s11207-016-0922-1 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_47 GBV_ILN_70 AR 291 2016 6 28 06 1647-1663 |
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10.1007/s11207-016-0922-1 doi (DE-627)OLC2033620611 (DE-He213)s11207-016-0922-1-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Solov’ev, A. A. verfasserin aut Analytical Model of an Asymmetric Sunspot with a Steady Plasma Flow in its Penumbra 2016 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2016 Abstract A new exact analytical solution to the stationary problem of ideal magnetohydrodynamics is derived for an unipolar asymmetric sunspot immersed in a realistic solar atmosphere. The radial and vertical profiles of pressure, plasma density, and temperature in the visible layers of the sunspot are calculated. The reduction in plasma density in the magnetic funnel of the sunspot, corresponding to the Wilson depression, is also obtained. The magnetic structure of the sunspot is given analytically in a realistic way: a part of the magnetic flux of the sunspot approaches the surrounding photosphere at the outer edge of the penumbra. The magnetic field of the sunspot is not assumed to be axially symmetric. For the first time, the angular dependence of the physical variables in this model allows us to simulate not only a deviation from the circular shape of the sunspot, but also a fine filamentary structure of the sunspot penumbra. The Alfvén Mach number (the ratio of the plasma speed to the Alfvén speed) is zero at the center of the sunspot and rises slowly toward the periphery of the sunspot; this corresponds to the structure of the Evershed flow in the penumbra. The Evershed flow in our model is mainly concentrated in dark penumbral filaments, as is observed. Sun Sunspots Magnetic field Model Umbra Penumbra Kirichek, E. A. aut Enthalten in Solar physics Springer Netherlands, 1967 291(2016), 6 vom: 28. Juni, Seite 1647-1663 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:291 year:2016 number:6 day:28 month:06 pages:1647-1663 https://doi.org/10.1007/s11207-016-0922-1 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_47 GBV_ILN_70 AR 291 2016 6 28 06 1647-1663 |
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Analytical Model of an Asymmetric Sunspot with a Steady Plasma Flow in its Penumbra |
| abstract |
Abstract A new exact analytical solution to the stationary problem of ideal magnetohydrodynamics is derived for an unipolar asymmetric sunspot immersed in a realistic solar atmosphere. The radial and vertical profiles of pressure, plasma density, and temperature in the visible layers of the sunspot are calculated. The reduction in plasma density in the magnetic funnel of the sunspot, corresponding to the Wilson depression, is also obtained. The magnetic structure of the sunspot is given analytically in a realistic way: a part of the magnetic flux of the sunspot approaches the surrounding photosphere at the outer edge of the penumbra. The magnetic field of the sunspot is not assumed to be axially symmetric. For the first time, the angular dependence of the physical variables in this model allows us to simulate not only a deviation from the circular shape of the sunspot, but also a fine filamentary structure of the sunspot penumbra. The Alfvén Mach number (the ratio of the plasma speed to the Alfvén speed) is zero at the center of the sunspot and rises slowly toward the periphery of the sunspot; this corresponds to the structure of the Evershed flow in the penumbra. The Evershed flow in our model is mainly concentrated in dark penumbral filaments, as is observed. © Springer Science+Business Media Dordrecht 2016 |
| abstractGer |
Abstract A new exact analytical solution to the stationary problem of ideal magnetohydrodynamics is derived for an unipolar asymmetric sunspot immersed in a realistic solar atmosphere. The radial and vertical profiles of pressure, plasma density, and temperature in the visible layers of the sunspot are calculated. The reduction in plasma density in the magnetic funnel of the sunspot, corresponding to the Wilson depression, is also obtained. The magnetic structure of the sunspot is given analytically in a realistic way: a part of the magnetic flux of the sunspot approaches the surrounding photosphere at the outer edge of the penumbra. The magnetic field of the sunspot is not assumed to be axially symmetric. For the first time, the angular dependence of the physical variables in this model allows us to simulate not only a deviation from the circular shape of the sunspot, but also a fine filamentary structure of the sunspot penumbra. The Alfvén Mach number (the ratio of the plasma speed to the Alfvén speed) is zero at the center of the sunspot and rises slowly toward the periphery of the sunspot; this corresponds to the structure of the Evershed flow in the penumbra. The Evershed flow in our model is mainly concentrated in dark penumbral filaments, as is observed. © Springer Science+Business Media Dordrecht 2016 |
| abstract_unstemmed |
Abstract A new exact analytical solution to the stationary problem of ideal magnetohydrodynamics is derived for an unipolar asymmetric sunspot immersed in a realistic solar atmosphere. The radial and vertical profiles of pressure, plasma density, and temperature in the visible layers of the sunspot are calculated. The reduction in plasma density in the magnetic funnel of the sunspot, corresponding to the Wilson depression, is also obtained. The magnetic structure of the sunspot is given analytically in a realistic way: a part of the magnetic flux of the sunspot approaches the surrounding photosphere at the outer edge of the penumbra. The magnetic field of the sunspot is not assumed to be axially symmetric. For the first time, the angular dependence of the physical variables in this model allows us to simulate not only a deviation from the circular shape of the sunspot, but also a fine filamentary structure of the sunspot penumbra. The Alfvén Mach number (the ratio of the plasma speed to the Alfvén speed) is zero at the center of the sunspot and rises slowly toward the periphery of the sunspot; this corresponds to the structure of the Evershed flow in the penumbra. The Evershed flow in our model is mainly concentrated in dark penumbral filaments, as is observed. © Springer Science+Business Media Dordrecht 2016 |
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| title_short |
Analytical Model of an Asymmetric Sunspot with a Steady Plasma Flow in its Penumbra |
| url |
https://doi.org/10.1007/s11207-016-0922-1 |
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| author2 |
Kirichek, E. A. |
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Kirichek, E. A. |
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| doi_str |
10.1007/s11207-016-0922-1 |
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2024-07-03T17:44:33.646Z |
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