The geometrical height-scale and the pressure equilibrium in the sunspot umbra
Abstract Spectra of spots very near to the solar limb (limb distance ≈ 8″) are used to determine the height difference between the levels of formation of the continuum and the line cores of 60 medium-strong Fraunhofer lines. For all lines (with Rowland Intensity < 10), this difference is < 1″...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Mattig, W. [verfasserIn] |
|---|
| Format: |
Artikel |
|---|---|
| Sprache: |
Englisch |
| Erschienen: |
1969 |
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| Schlagwörter: |
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| Anmerkung: |
© D. Reidel Publishing Company 1969 |
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| Übergeordnetes Werk: |
Enthalten in: Solar physics - Kluwer Academic Publishers, 1967, 8(1969), 2 vom: Aug., Seite 291-309 |
|---|---|
| Übergeordnetes Werk: |
volume:8 ; year:1969 ; number:2 ; month:08 ; pages:291-309 |
| Links: |
|---|
| DOI / URN: |
10.1007/BF00155377 |
|---|
| Katalog-ID: |
OLC2033519848 |
|---|
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| 245 | 1 | 0 | |a The geometrical height-scale and the pressure equilibrium in the sunspot umbra |
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| 520 | |a Abstract Spectra of spots very near to the solar limb (limb distance ≈ 8″) are used to determine the height difference between the levels of formation of the continuum and the line cores of 60 medium-strong Fraunhofer lines. For all lines (with Rowland Intensity < 10), this difference is < 1″ (= 725 km) and well correlated with the Rowland intensity. The line absorption coefficient is calculated for some lines with known oscillator strength. This gives a possibility to deduce a value for the scale height of the umbra, which is found to be about 100 km, thus being equal to the photospheric scale height. Pure hydrostatic equilibrium exists, therefore, in the umbra, and vertical magnetic forces are negligible. Other methods for determining the scale height are discussed for comparison. The horizontal pressure equilibrium is discussed by taking into account the Wilson effect, and by neglecting dynamic terms (flow of matter). The magnetic field is confirmed to be force-free in higher layers (chromosphere). The pressure difference umbra-photosphere increases towards deeper layers, having a maximum at $ τ^{*} $ ∼- 1 which corresponds to about two times the magnetic pressure H2/8π. If rotational symmetry of the field is assumed, this can be explained by a minimum radius of curvature of the field lines of 1/4 spot radius. | ||
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10.1007/BF00155377 doi (DE-627)OLC2033519848 (DE-He213)BF00155377-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Mattig, W. verfasserin aut The geometrical height-scale and the pressure equilibrium in the sunspot umbra 1969 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1969 Abstract Spectra of spots very near to the solar limb (limb distance ≈ 8″) are used to determine the height difference between the levels of formation of the continuum and the line cores of 60 medium-strong Fraunhofer lines. For all lines (with Rowland Intensity < 10), this difference is < 1″ (= 725 km) and well correlated with the Rowland intensity. The line absorption coefficient is calculated for some lines with known oscillator strength. This gives a possibility to deduce a value for the scale height of the umbra, which is found to be about 100 km, thus being equal to the photospheric scale height. Pure hydrostatic equilibrium exists, therefore, in the umbra, and vertical magnetic forces are negligible. Other methods for determining the scale height are discussed for comparison. The horizontal pressure equilibrium is discussed by taking into account the Wilson effect, and by neglecting dynamic terms (flow of matter). The magnetic field is confirmed to be force-free in higher layers (chromosphere). The pressure difference umbra-photosphere increases towards deeper layers, having a maximum at $ τ^{*} $ ∼- 1 which corresponds to about two times the magnetic pressure H2/8π. If rotational symmetry of the field is assumed, this can be explained by a minimum radius of curvature of the field lines of 1/4 spot radius. Field Line Magnetic Force Oscillator Strength Rotational Symmetry Pressure Equilibrium Enthalten in Solar physics Kluwer Academic Publishers, 1967 8(1969), 2 vom: Aug., Seite 291-309 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:8 year:1969 number:2 month:08 pages:291-309 https://doi.org/10.1007/BF00155377 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_170 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4306 AR 8 1969 2 08 291-309 |
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10.1007/BF00155377 doi (DE-627)OLC2033519848 (DE-He213)BF00155377-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Mattig, W. verfasserin aut The geometrical height-scale and the pressure equilibrium in the sunspot umbra 1969 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1969 Abstract Spectra of spots very near to the solar limb (limb distance ≈ 8″) are used to determine the height difference between the levels of formation of the continuum and the line cores of 60 medium-strong Fraunhofer lines. For all lines (with Rowland Intensity < 10), this difference is < 1″ (= 725 km) and well correlated with the Rowland intensity. The line absorption coefficient is calculated for some lines with known oscillator strength. This gives a possibility to deduce a value for the scale height of the umbra, which is found to be about 100 km, thus being equal to the photospheric scale height. Pure hydrostatic equilibrium exists, therefore, in the umbra, and vertical magnetic forces are negligible. Other methods for determining the scale height are discussed for comparison. The horizontal pressure equilibrium is discussed by taking into account the Wilson effect, and by neglecting dynamic terms (flow of matter). The magnetic field is confirmed to be force-free in higher layers (chromosphere). The pressure difference umbra-photosphere increases towards deeper layers, having a maximum at $ τ^{*} $ ∼- 1 which corresponds to about two times the magnetic pressure H2/8π. If rotational symmetry of the field is assumed, this can be explained by a minimum radius of curvature of the field lines of 1/4 spot radius. Field Line Magnetic Force Oscillator Strength Rotational Symmetry Pressure Equilibrium Enthalten in Solar physics Kluwer Academic Publishers, 1967 8(1969), 2 vom: Aug., Seite 291-309 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:8 year:1969 number:2 month:08 pages:291-309 https://doi.org/10.1007/BF00155377 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_170 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4306 AR 8 1969 2 08 291-309 |
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10.1007/BF00155377 doi (DE-627)OLC2033519848 (DE-He213)BF00155377-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Mattig, W. verfasserin aut The geometrical height-scale and the pressure equilibrium in the sunspot umbra 1969 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1969 Abstract Spectra of spots very near to the solar limb (limb distance ≈ 8″) are used to determine the height difference between the levels of formation of the continuum and the line cores of 60 medium-strong Fraunhofer lines. For all lines (with Rowland Intensity < 10), this difference is < 1″ (= 725 km) and well correlated with the Rowland intensity. The line absorption coefficient is calculated for some lines with known oscillator strength. This gives a possibility to deduce a value for the scale height of the umbra, which is found to be about 100 km, thus being equal to the photospheric scale height. Pure hydrostatic equilibrium exists, therefore, in the umbra, and vertical magnetic forces are negligible. Other methods for determining the scale height are discussed for comparison. The horizontal pressure equilibrium is discussed by taking into account the Wilson effect, and by neglecting dynamic terms (flow of matter). The magnetic field is confirmed to be force-free in higher layers (chromosphere). The pressure difference umbra-photosphere increases towards deeper layers, having a maximum at $ τ^{*} $ ∼- 1 which corresponds to about two times the magnetic pressure H2/8π. If rotational symmetry of the field is assumed, this can be explained by a minimum radius of curvature of the field lines of 1/4 spot radius. Field Line Magnetic Force Oscillator Strength Rotational Symmetry Pressure Equilibrium Enthalten in Solar physics Kluwer Academic Publishers, 1967 8(1969), 2 vom: Aug., Seite 291-309 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:8 year:1969 number:2 month:08 pages:291-309 https://doi.org/10.1007/BF00155377 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_170 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4306 AR 8 1969 2 08 291-309 |
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10.1007/BF00155377 doi (DE-627)OLC2033519848 (DE-He213)BF00155377-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Mattig, W. verfasserin aut The geometrical height-scale and the pressure equilibrium in the sunspot umbra 1969 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1969 Abstract Spectra of spots very near to the solar limb (limb distance ≈ 8″) are used to determine the height difference between the levels of formation of the continuum and the line cores of 60 medium-strong Fraunhofer lines. For all lines (with Rowland Intensity < 10), this difference is < 1″ (= 725 km) and well correlated with the Rowland intensity. The line absorption coefficient is calculated for some lines with known oscillator strength. This gives a possibility to deduce a value for the scale height of the umbra, which is found to be about 100 km, thus being equal to the photospheric scale height. Pure hydrostatic equilibrium exists, therefore, in the umbra, and vertical magnetic forces are negligible. Other methods for determining the scale height are discussed for comparison. The horizontal pressure equilibrium is discussed by taking into account the Wilson effect, and by neglecting dynamic terms (flow of matter). The magnetic field is confirmed to be force-free in higher layers (chromosphere). The pressure difference umbra-photosphere increases towards deeper layers, having a maximum at $ τ^{*} $ ∼- 1 which corresponds to about two times the magnetic pressure H2/8π. If rotational symmetry of the field is assumed, this can be explained by a minimum radius of curvature of the field lines of 1/4 spot radius. Field Line Magnetic Force Oscillator Strength Rotational Symmetry Pressure Equilibrium Enthalten in Solar physics Kluwer Academic Publishers, 1967 8(1969), 2 vom: Aug., Seite 291-309 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:8 year:1969 number:2 month:08 pages:291-309 https://doi.org/10.1007/BF00155377 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_170 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4306 AR 8 1969 2 08 291-309 |
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10.1007/BF00155377 doi (DE-627)OLC2033519848 (DE-He213)BF00155377-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Mattig, W. verfasserin aut The geometrical height-scale and the pressure equilibrium in the sunspot umbra 1969 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1969 Abstract Spectra of spots very near to the solar limb (limb distance ≈ 8″) are used to determine the height difference between the levels of formation of the continuum and the line cores of 60 medium-strong Fraunhofer lines. For all lines (with Rowland Intensity < 10), this difference is < 1″ (= 725 km) and well correlated with the Rowland intensity. The line absorption coefficient is calculated for some lines with known oscillator strength. This gives a possibility to deduce a value for the scale height of the umbra, which is found to be about 100 km, thus being equal to the photospheric scale height. Pure hydrostatic equilibrium exists, therefore, in the umbra, and vertical magnetic forces are negligible. Other methods for determining the scale height are discussed for comparison. The horizontal pressure equilibrium is discussed by taking into account the Wilson effect, and by neglecting dynamic terms (flow of matter). The magnetic field is confirmed to be force-free in higher layers (chromosphere). The pressure difference umbra-photosphere increases towards deeper layers, having a maximum at $ τ^{*} $ ∼- 1 which corresponds to about two times the magnetic pressure H2/8π. If rotational symmetry of the field is assumed, this can be explained by a minimum radius of curvature of the field lines of 1/4 spot radius. Field Line Magnetic Force Oscillator Strength Rotational Symmetry Pressure Equilibrium Enthalten in Solar physics Kluwer Academic Publishers, 1967 8(1969), 2 vom: Aug., Seite 291-309 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:8 year:1969 number:2 month:08 pages:291-309 https://doi.org/10.1007/BF00155377 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_170 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4306 AR 8 1969 2 08 291-309 |
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530 VZ 16,12 ssgn The geometrical height-scale and the pressure equilibrium in the sunspot umbra Field Line Magnetic Force Oscillator Strength Rotational Symmetry Pressure Equilibrium |
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ddc 530 ssgn 16,12 misc Field Line misc Magnetic Force misc Oscillator Strength misc Rotational Symmetry misc Pressure Equilibrium |
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The geometrical height-scale and the pressure equilibrium in the sunspot umbra |
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The geometrical height-scale and the pressure equilibrium in the sunspot umbra |
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Mattig, W. |
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Solar physics |
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Mattig, W. |
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the geometrical height-scale and the pressure equilibrium in the sunspot umbra |
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The geometrical height-scale and the pressure equilibrium in the sunspot umbra |
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Abstract Spectra of spots very near to the solar limb (limb distance ≈ 8″) are used to determine the height difference between the levels of formation of the continuum and the line cores of 60 medium-strong Fraunhofer lines. For all lines (with Rowland Intensity < 10), this difference is < 1″ (= 725 km) and well correlated with the Rowland intensity. The line absorption coefficient is calculated for some lines with known oscillator strength. This gives a possibility to deduce a value for the scale height of the umbra, which is found to be about 100 km, thus being equal to the photospheric scale height. Pure hydrostatic equilibrium exists, therefore, in the umbra, and vertical magnetic forces are negligible. Other methods for determining the scale height are discussed for comparison. The horizontal pressure equilibrium is discussed by taking into account the Wilson effect, and by neglecting dynamic terms (flow of matter). The magnetic field is confirmed to be force-free in higher layers (chromosphere). The pressure difference umbra-photosphere increases towards deeper layers, having a maximum at $ τ^{*} $ ∼- 1 which corresponds to about two times the magnetic pressure H2/8π. If rotational symmetry of the field is assumed, this can be explained by a minimum radius of curvature of the field lines of 1/4 spot radius. © D. Reidel Publishing Company 1969 |
| abstractGer |
Abstract Spectra of spots very near to the solar limb (limb distance ≈ 8″) are used to determine the height difference between the levels of formation of the continuum and the line cores of 60 medium-strong Fraunhofer lines. For all lines (with Rowland Intensity < 10), this difference is < 1″ (= 725 km) and well correlated with the Rowland intensity. The line absorption coefficient is calculated for some lines with known oscillator strength. This gives a possibility to deduce a value for the scale height of the umbra, which is found to be about 100 km, thus being equal to the photospheric scale height. Pure hydrostatic equilibrium exists, therefore, in the umbra, and vertical magnetic forces are negligible. Other methods for determining the scale height are discussed for comparison. The horizontal pressure equilibrium is discussed by taking into account the Wilson effect, and by neglecting dynamic terms (flow of matter). The magnetic field is confirmed to be force-free in higher layers (chromosphere). The pressure difference umbra-photosphere increases towards deeper layers, having a maximum at $ τ^{*} $ ∼- 1 which corresponds to about two times the magnetic pressure H2/8π. If rotational symmetry of the field is assumed, this can be explained by a minimum radius of curvature of the field lines of 1/4 spot radius. © D. Reidel Publishing Company 1969 |
| abstract_unstemmed |
Abstract Spectra of spots very near to the solar limb (limb distance ≈ 8″) are used to determine the height difference between the levels of formation of the continuum and the line cores of 60 medium-strong Fraunhofer lines. For all lines (with Rowland Intensity < 10), this difference is < 1″ (= 725 km) and well correlated with the Rowland intensity. The line absorption coefficient is calculated for some lines with known oscillator strength. This gives a possibility to deduce a value for the scale height of the umbra, which is found to be about 100 km, thus being equal to the photospheric scale height. Pure hydrostatic equilibrium exists, therefore, in the umbra, and vertical magnetic forces are negligible. Other methods for determining the scale height are discussed for comparison. The horizontal pressure equilibrium is discussed by taking into account the Wilson effect, and by neglecting dynamic terms (flow of matter). The magnetic field is confirmed to be force-free in higher layers (chromosphere). The pressure difference umbra-photosphere increases towards deeper layers, having a maximum at $ τ^{*} $ ∼- 1 which corresponds to about two times the magnetic pressure H2/8π. If rotational symmetry of the field is assumed, this can be explained by a minimum radius of curvature of the field lines of 1/4 spot radius. © D. Reidel Publishing Company 1969 |
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The geometrical height-scale and the pressure equilibrium in the sunspot umbra |
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