On convection in the sun
Abstract Convective motions driven by a superadiabatic temperature gradient in a viscous thermally conductive medium are considered. Approximate linearized equations governing the perturbation are derived under the following conditions: (i) The ratio of the excess temperature gradient over the adiab...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Vandakurov, Yu. V. [verfasserIn] |
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| Format: |
Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
1975 |
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| Schlagwörter: |
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| Anmerkung: |
© D. Reidel Publishing Company 1975 |
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| Übergeordnetes Werk: |
Enthalten in: Solar physics - Kluwer Academic Publishers, 1967, 40(1975), 1 vom: Jan., Seite 3-21 |
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| Übergeordnetes Werk: |
volume:40 ; year:1975 ; number:1 ; month:01 ; pages:3-21 |
| Links: |
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| DOI / URN: |
10.1007/BF00183148 |
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| Katalog-ID: |
OLC2033536289 |
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| 520 | |a Abstract Convective motions driven by a superadiabatic temperature gradient in a viscous thermally conductive medium are considered. Approximate linearized equations governing the perturbation are derived under the following conditions: (i) The ratio of the excess temperature gradient over the adiabatic gradient is small compared with the gradient itself, (ii) The perturbation is of low-frequency type, (iii) The rotation is slow. Only the convective mode is described by these equations (as in the Boussinesq approximation), and the equations are valid for compressible configurations with any ratio between the scale heights of the equilibrium and perturbed quantities. Results of a numerical calculation of unstable perturbations for configurations with a large density stratification are given. They show that under conditions appropriate for the solar convection zone an extremely strong instability is expected to occur if the mixing length is assumed to be equal to 1.5 times the pressure scale height. The horizontal scale of the instability is intermediate between those of granulation and supergranulation. The larger the mixing length, the smaller the growth rate of the instability, and the larger its horizontal scale. Therefore it seems possible to adjust the mixing length to obtain the characteristics corresponding to those of the solar supergranulation. The possible origin of the granulation as an instability in a subsurface zone, where a local increase in the density scale height takes place, is also discussed. To achieve agreement with observations, it seems necessary to assume that the ratio of the mixing length to pressure scale height is an increasing function of the pressure. | ||
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10.1007/BF00183148 doi (DE-627)OLC2033536289 (DE-He213)BF00183148-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Vandakurov, Yu. V. verfasserin aut On convection in the sun 1975 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1975 Abstract Convective motions driven by a superadiabatic temperature gradient in a viscous thermally conductive medium are considered. Approximate linearized equations governing the perturbation are derived under the following conditions: (i) The ratio of the excess temperature gradient over the adiabatic gradient is small compared with the gradient itself, (ii) The perturbation is of low-frequency type, (iii) The rotation is slow. Only the convective mode is described by these equations (as in the Boussinesq approximation), and the equations are valid for compressible configurations with any ratio between the scale heights of the equilibrium and perturbed quantities. Results of a numerical calculation of unstable perturbations for configurations with a large density stratification are given. They show that under conditions appropriate for the solar convection zone an extremely strong instability is expected to occur if the mixing length is assumed to be equal to 1.5 times the pressure scale height. The horizontal scale of the instability is intermediate between those of granulation and supergranulation. The larger the mixing length, the smaller the growth rate of the instability, and the larger its horizontal scale. Therefore it seems possible to adjust the mixing length to obtain the characteristics corresponding to those of the solar supergranulation. The possible origin of the granulation as an instability in a subsurface zone, where a local increase in the density scale height takes place, is also discussed. To achieve agreement with observations, it seems necessary to assume that the ratio of the mixing length to pressure scale height is an increasing function of the pressure. Convection Zone Scale Height Horizontal Scale Boussinesq Approximation Density Stratification Enthalten in Solar physics Kluwer Academic Publishers, 1967 40(1975), 1 vom: Jan., Seite 3-21 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:40 year:1975 number:1 month:01 pages:3-21 https://doi.org/10.1007/BF00183148 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4305 GBV_ILN_4306 AR 40 1975 1 01 3-21 |
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10.1007/BF00183148 doi (DE-627)OLC2033536289 (DE-He213)BF00183148-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Vandakurov, Yu. V. verfasserin aut On convection in the sun 1975 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1975 Abstract Convective motions driven by a superadiabatic temperature gradient in a viscous thermally conductive medium are considered. Approximate linearized equations governing the perturbation are derived under the following conditions: (i) The ratio of the excess temperature gradient over the adiabatic gradient is small compared with the gradient itself, (ii) The perturbation is of low-frequency type, (iii) The rotation is slow. Only the convective mode is described by these equations (as in the Boussinesq approximation), and the equations are valid for compressible configurations with any ratio between the scale heights of the equilibrium and perturbed quantities. Results of a numerical calculation of unstable perturbations for configurations with a large density stratification are given. They show that under conditions appropriate for the solar convection zone an extremely strong instability is expected to occur if the mixing length is assumed to be equal to 1.5 times the pressure scale height. The horizontal scale of the instability is intermediate between those of granulation and supergranulation. The larger the mixing length, the smaller the growth rate of the instability, and the larger its horizontal scale. Therefore it seems possible to adjust the mixing length to obtain the characteristics corresponding to those of the solar supergranulation. The possible origin of the granulation as an instability in a subsurface zone, where a local increase in the density scale height takes place, is also discussed. To achieve agreement with observations, it seems necessary to assume that the ratio of the mixing length to pressure scale height is an increasing function of the pressure. Convection Zone Scale Height Horizontal Scale Boussinesq Approximation Density Stratification Enthalten in Solar physics Kluwer Academic Publishers, 1967 40(1975), 1 vom: Jan., Seite 3-21 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:40 year:1975 number:1 month:01 pages:3-21 https://doi.org/10.1007/BF00183148 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4305 GBV_ILN_4306 AR 40 1975 1 01 3-21 |
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10.1007/BF00183148 doi (DE-627)OLC2033536289 (DE-He213)BF00183148-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Vandakurov, Yu. V. verfasserin aut On convection in the sun 1975 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1975 Abstract Convective motions driven by a superadiabatic temperature gradient in a viscous thermally conductive medium are considered. Approximate linearized equations governing the perturbation are derived under the following conditions: (i) The ratio of the excess temperature gradient over the adiabatic gradient is small compared with the gradient itself, (ii) The perturbation is of low-frequency type, (iii) The rotation is slow. Only the convective mode is described by these equations (as in the Boussinesq approximation), and the equations are valid for compressible configurations with any ratio between the scale heights of the equilibrium and perturbed quantities. Results of a numerical calculation of unstable perturbations for configurations with a large density stratification are given. They show that under conditions appropriate for the solar convection zone an extremely strong instability is expected to occur if the mixing length is assumed to be equal to 1.5 times the pressure scale height. The horizontal scale of the instability is intermediate between those of granulation and supergranulation. The larger the mixing length, the smaller the growth rate of the instability, and the larger its horizontal scale. Therefore it seems possible to adjust the mixing length to obtain the characteristics corresponding to those of the solar supergranulation. The possible origin of the granulation as an instability in a subsurface zone, where a local increase in the density scale height takes place, is also discussed. To achieve agreement with observations, it seems necessary to assume that the ratio of the mixing length to pressure scale height is an increasing function of the pressure. Convection Zone Scale Height Horizontal Scale Boussinesq Approximation Density Stratification Enthalten in Solar physics Kluwer Academic Publishers, 1967 40(1975), 1 vom: Jan., Seite 3-21 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:40 year:1975 number:1 month:01 pages:3-21 https://doi.org/10.1007/BF00183148 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4305 GBV_ILN_4306 AR 40 1975 1 01 3-21 |
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10.1007/BF00183148 doi (DE-627)OLC2033536289 (DE-He213)BF00183148-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Vandakurov, Yu. V. verfasserin aut On convection in the sun 1975 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1975 Abstract Convective motions driven by a superadiabatic temperature gradient in a viscous thermally conductive medium are considered. Approximate linearized equations governing the perturbation are derived under the following conditions: (i) The ratio of the excess temperature gradient over the adiabatic gradient is small compared with the gradient itself, (ii) The perturbation is of low-frequency type, (iii) The rotation is slow. Only the convective mode is described by these equations (as in the Boussinesq approximation), and the equations are valid for compressible configurations with any ratio between the scale heights of the equilibrium and perturbed quantities. Results of a numerical calculation of unstable perturbations for configurations with a large density stratification are given. They show that under conditions appropriate for the solar convection zone an extremely strong instability is expected to occur if the mixing length is assumed to be equal to 1.5 times the pressure scale height. The horizontal scale of the instability is intermediate between those of granulation and supergranulation. The larger the mixing length, the smaller the growth rate of the instability, and the larger its horizontal scale. Therefore it seems possible to adjust the mixing length to obtain the characteristics corresponding to those of the solar supergranulation. The possible origin of the granulation as an instability in a subsurface zone, where a local increase in the density scale height takes place, is also discussed. To achieve agreement with observations, it seems necessary to assume that the ratio of the mixing length to pressure scale height is an increasing function of the pressure. Convection Zone Scale Height Horizontal Scale Boussinesq Approximation Density Stratification Enthalten in Solar physics Kluwer Academic Publishers, 1967 40(1975), 1 vom: Jan., Seite 3-21 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:40 year:1975 number:1 month:01 pages:3-21 https://doi.org/10.1007/BF00183148 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4305 GBV_ILN_4306 AR 40 1975 1 01 3-21 |
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10.1007/BF00183148 doi (DE-627)OLC2033536289 (DE-He213)BF00183148-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Vandakurov, Yu. V. verfasserin aut On convection in the sun 1975 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1975 Abstract Convective motions driven by a superadiabatic temperature gradient in a viscous thermally conductive medium are considered. Approximate linearized equations governing the perturbation are derived under the following conditions: (i) The ratio of the excess temperature gradient over the adiabatic gradient is small compared with the gradient itself, (ii) The perturbation is of low-frequency type, (iii) The rotation is slow. Only the convective mode is described by these equations (as in the Boussinesq approximation), and the equations are valid for compressible configurations with any ratio between the scale heights of the equilibrium and perturbed quantities. Results of a numerical calculation of unstable perturbations for configurations with a large density stratification are given. They show that under conditions appropriate for the solar convection zone an extremely strong instability is expected to occur if the mixing length is assumed to be equal to 1.5 times the pressure scale height. The horizontal scale of the instability is intermediate between those of granulation and supergranulation. The larger the mixing length, the smaller the growth rate of the instability, and the larger its horizontal scale. Therefore it seems possible to adjust the mixing length to obtain the characteristics corresponding to those of the solar supergranulation. The possible origin of the granulation as an instability in a subsurface zone, where a local increase in the density scale height takes place, is also discussed. To achieve agreement with observations, it seems necessary to assume that the ratio of the mixing length to pressure scale height is an increasing function of the pressure. Convection Zone Scale Height Horizontal Scale Boussinesq Approximation Density Stratification Enthalten in Solar physics Kluwer Academic Publishers, 1967 40(1975), 1 vom: Jan., Seite 3-21 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:40 year:1975 number:1 month:01 pages:3-21 https://doi.org/10.1007/BF00183148 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4305 GBV_ILN_4306 AR 40 1975 1 01 3-21 |
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530 VZ 16,12 ssgn On convection in the sun Convection Zone Scale Height Horizontal Scale Boussinesq Approximation Density Stratification |
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On convection in the sun |
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On convection in the sun |
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on convection in the sun |
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On convection in the sun |
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Abstract Convective motions driven by a superadiabatic temperature gradient in a viscous thermally conductive medium are considered. Approximate linearized equations governing the perturbation are derived under the following conditions: (i) The ratio of the excess temperature gradient over the adiabatic gradient is small compared with the gradient itself, (ii) The perturbation is of low-frequency type, (iii) The rotation is slow. Only the convective mode is described by these equations (as in the Boussinesq approximation), and the equations are valid for compressible configurations with any ratio between the scale heights of the equilibrium and perturbed quantities. Results of a numerical calculation of unstable perturbations for configurations with a large density stratification are given. They show that under conditions appropriate for the solar convection zone an extremely strong instability is expected to occur if the mixing length is assumed to be equal to 1.5 times the pressure scale height. The horizontal scale of the instability is intermediate between those of granulation and supergranulation. The larger the mixing length, the smaller the growth rate of the instability, and the larger its horizontal scale. Therefore it seems possible to adjust the mixing length to obtain the characteristics corresponding to those of the solar supergranulation. The possible origin of the granulation as an instability in a subsurface zone, where a local increase in the density scale height takes place, is also discussed. To achieve agreement with observations, it seems necessary to assume that the ratio of the mixing length to pressure scale height is an increasing function of the pressure. © D. Reidel Publishing Company 1975 |
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Abstract Convective motions driven by a superadiabatic temperature gradient in a viscous thermally conductive medium are considered. Approximate linearized equations governing the perturbation are derived under the following conditions: (i) The ratio of the excess temperature gradient over the adiabatic gradient is small compared with the gradient itself, (ii) The perturbation is of low-frequency type, (iii) The rotation is slow. Only the convective mode is described by these equations (as in the Boussinesq approximation), and the equations are valid for compressible configurations with any ratio between the scale heights of the equilibrium and perturbed quantities. Results of a numerical calculation of unstable perturbations for configurations with a large density stratification are given. They show that under conditions appropriate for the solar convection zone an extremely strong instability is expected to occur if the mixing length is assumed to be equal to 1.5 times the pressure scale height. The horizontal scale of the instability is intermediate between those of granulation and supergranulation. The larger the mixing length, the smaller the growth rate of the instability, and the larger its horizontal scale. Therefore it seems possible to adjust the mixing length to obtain the characteristics corresponding to those of the solar supergranulation. The possible origin of the granulation as an instability in a subsurface zone, where a local increase in the density scale height takes place, is also discussed. To achieve agreement with observations, it seems necessary to assume that the ratio of the mixing length to pressure scale height is an increasing function of the pressure. © D. Reidel Publishing Company 1975 |
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Abstract Convective motions driven by a superadiabatic temperature gradient in a viscous thermally conductive medium are considered. Approximate linearized equations governing the perturbation are derived under the following conditions: (i) The ratio of the excess temperature gradient over the adiabatic gradient is small compared with the gradient itself, (ii) The perturbation is of low-frequency type, (iii) The rotation is slow. Only the convective mode is described by these equations (as in the Boussinesq approximation), and the equations are valid for compressible configurations with any ratio between the scale heights of the equilibrium and perturbed quantities. Results of a numerical calculation of unstable perturbations for configurations with a large density stratification are given. They show that under conditions appropriate for the solar convection zone an extremely strong instability is expected to occur if the mixing length is assumed to be equal to 1.5 times the pressure scale height. The horizontal scale of the instability is intermediate between those of granulation and supergranulation. The larger the mixing length, the smaller the growth rate of the instability, and the larger its horizontal scale. Therefore it seems possible to adjust the mixing length to obtain the characteristics corresponding to those of the solar supergranulation. The possible origin of the granulation as an instability in a subsurface zone, where a local increase in the density scale height takes place, is also discussed. To achieve agreement with observations, it seems necessary to assume that the ratio of the mixing length to pressure scale height is an increasing function of the pressure. © D. Reidel Publishing Company 1975 |
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