Observations of stray-light and sunspot intensities during the Mercury transit of 1970 May 9
Abstract In order to test the usual method for correcting sunspot intensity measurements for stray light, we have measured, during the Mercury transit of 1970 May 9, the intensities of Mercury, a sunspot umbra, and the aureole. The direct observations result in Mercury intensities < 0.06 I⊙ and a...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Mattig, W. [verfasserIn] |
|---|
| Format: |
Artikel |
|---|---|
| Sprache: |
Englisch |
| Erschienen: |
1971 |
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| Schlagwörter: |
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| Anmerkung: |
© D. Reidel Publishing Company 1971 |
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| Übergeordnetes Werk: |
Enthalten in: Solar physics - Kluwer Academic Publishers, 1967, 18(1971), 3 vom: Juli, Seite 434-442 |
|---|---|
| Übergeordnetes Werk: |
volume:18 ; year:1971 ; number:3 ; month:07 ; pages:434-442 |
| Links: |
|---|
| DOI / URN: |
10.1007/BF00149065 |
|---|
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OLC2033525163 |
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| 520 | |a Abstract In order to test the usual method for correcting sunspot intensity measurements for stray light, we have measured, during the Mercury transit of 1970 May 9, the intensities of Mercury, a sunspot umbra, and the aureole. The direct observations result in Mercury intensities < 0.06 I⊙ and aureole intensities <0.01 I⊙. The stray light correction to the spot intensities has been <(0.03 ± 0.01) I⊙. The main contribution to the stray light on the solar disc is shown to be produced by a spread-function with a half width of 10 arc sec. Consequently, for stray light corrections the range R ⩽ R⊙ + + 20″ in the aureole has to be measured very precisely; furthermore, a remarkable fraction of the stray light in the center of an umbra originates from the surrounding penumbra. | ||
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10.1007/BF00149065 doi (DE-627)OLC2033525163 (DE-He213)BF00149065-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Mattig, W. verfasserin aut Observations of stray-light and sunspot intensities during the Mercury transit of 1970 May 9 1971 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1971 Abstract In order to test the usual method for correcting sunspot intensity measurements for stray light, we have measured, during the Mercury transit of 1970 May 9, the intensities of Mercury, a sunspot umbra, and the aureole. The direct observations result in Mercury intensities < 0.06 I⊙ and aureole intensities <0.01 I⊙. The stray light correction to the spot intensities has been <(0.03 ± 0.01) I⊙. The main contribution to the stray light on the solar disc is shown to be produced by a spread-function with a half width of 10 arc sec. Consequently, for stray light corrections the range R ⩽ R⊙ + + 20″ in the aureole has to be measured very precisely; furthermore, a remarkable fraction of the stray light in the center of an umbra originates from the surrounding penumbra. Mercury Direct Observation Intensity Measurement Half Width Usual Method Enthalten in Solar physics Kluwer Academic Publishers, 1967 18(1971), 3 vom: Juli, Seite 434-442 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:18 year:1971 number:3 month:07 pages:434-442 https://doi.org/10.1007/BF00149065 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_4306 AR 18 1971 3 07 434-442 |
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10.1007/BF00149065 doi (DE-627)OLC2033525163 (DE-He213)BF00149065-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Mattig, W. verfasserin aut Observations of stray-light and sunspot intensities during the Mercury transit of 1970 May 9 1971 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1971 Abstract In order to test the usual method for correcting sunspot intensity measurements for stray light, we have measured, during the Mercury transit of 1970 May 9, the intensities of Mercury, a sunspot umbra, and the aureole. The direct observations result in Mercury intensities < 0.06 I⊙ and aureole intensities <0.01 I⊙. The stray light correction to the spot intensities has been <(0.03 ± 0.01) I⊙. The main contribution to the stray light on the solar disc is shown to be produced by a spread-function with a half width of 10 arc sec. Consequently, for stray light corrections the range R ⩽ R⊙ + + 20″ in the aureole has to be measured very precisely; furthermore, a remarkable fraction of the stray light in the center of an umbra originates from the surrounding penumbra. Mercury Direct Observation Intensity Measurement Half Width Usual Method Enthalten in Solar physics Kluwer Academic Publishers, 1967 18(1971), 3 vom: Juli, Seite 434-442 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:18 year:1971 number:3 month:07 pages:434-442 https://doi.org/10.1007/BF00149065 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_4306 AR 18 1971 3 07 434-442 |
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10.1007/BF00149065 doi (DE-627)OLC2033525163 (DE-He213)BF00149065-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Mattig, W. verfasserin aut Observations of stray-light and sunspot intensities during the Mercury transit of 1970 May 9 1971 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1971 Abstract In order to test the usual method for correcting sunspot intensity measurements for stray light, we have measured, during the Mercury transit of 1970 May 9, the intensities of Mercury, a sunspot umbra, and the aureole. The direct observations result in Mercury intensities < 0.06 I⊙ and aureole intensities <0.01 I⊙. The stray light correction to the spot intensities has been <(0.03 ± 0.01) I⊙. The main contribution to the stray light on the solar disc is shown to be produced by a spread-function with a half width of 10 arc sec. Consequently, for stray light corrections the range R ⩽ R⊙ + + 20″ in the aureole has to be measured very precisely; furthermore, a remarkable fraction of the stray light in the center of an umbra originates from the surrounding penumbra. Mercury Direct Observation Intensity Measurement Half Width Usual Method Enthalten in Solar physics Kluwer Academic Publishers, 1967 18(1971), 3 vom: Juli, Seite 434-442 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:18 year:1971 number:3 month:07 pages:434-442 https://doi.org/10.1007/BF00149065 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_4306 AR 18 1971 3 07 434-442 |
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10.1007/BF00149065 doi (DE-627)OLC2033525163 (DE-He213)BF00149065-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Mattig, W. verfasserin aut Observations of stray-light and sunspot intensities during the Mercury transit of 1970 May 9 1971 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1971 Abstract In order to test the usual method for correcting sunspot intensity measurements for stray light, we have measured, during the Mercury transit of 1970 May 9, the intensities of Mercury, a sunspot umbra, and the aureole. The direct observations result in Mercury intensities < 0.06 I⊙ and aureole intensities <0.01 I⊙. The stray light correction to the spot intensities has been <(0.03 ± 0.01) I⊙. The main contribution to the stray light on the solar disc is shown to be produced by a spread-function with a half width of 10 arc sec. Consequently, for stray light corrections the range R ⩽ R⊙ + + 20″ in the aureole has to be measured very precisely; furthermore, a remarkable fraction of the stray light in the center of an umbra originates from the surrounding penumbra. Mercury Direct Observation Intensity Measurement Half Width Usual Method Enthalten in Solar physics Kluwer Academic Publishers, 1967 18(1971), 3 vom: Juli, Seite 434-442 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:18 year:1971 number:3 month:07 pages:434-442 https://doi.org/10.1007/BF00149065 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_4306 AR 18 1971 3 07 434-442 |
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10.1007/BF00149065 doi (DE-627)OLC2033525163 (DE-He213)BF00149065-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Mattig, W. verfasserin aut Observations of stray-light and sunspot intensities during the Mercury transit of 1970 May 9 1971 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1971 Abstract In order to test the usual method for correcting sunspot intensity measurements for stray light, we have measured, during the Mercury transit of 1970 May 9, the intensities of Mercury, a sunspot umbra, and the aureole. The direct observations result in Mercury intensities < 0.06 I⊙ and aureole intensities <0.01 I⊙. The stray light correction to the spot intensities has been <(0.03 ± 0.01) I⊙. The main contribution to the stray light on the solar disc is shown to be produced by a spread-function with a half width of 10 arc sec. Consequently, for stray light corrections the range R ⩽ R⊙ + + 20″ in the aureole has to be measured very precisely; furthermore, a remarkable fraction of the stray light in the center of an umbra originates from the surrounding penumbra. Mercury Direct Observation Intensity Measurement Half Width Usual Method Enthalten in Solar physics Kluwer Academic Publishers, 1967 18(1971), 3 vom: Juli, Seite 434-442 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:18 year:1971 number:3 month:07 pages:434-442 https://doi.org/10.1007/BF00149065 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_4306 AR 18 1971 3 07 434-442 |
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observations of stray-light and sunspot intensities during the mercury transit of 1970 may 9 |
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Observations of stray-light and sunspot intensities during the Mercury transit of 1970 May 9 |
| abstract |
Abstract In order to test the usual method for correcting sunspot intensity measurements for stray light, we have measured, during the Mercury transit of 1970 May 9, the intensities of Mercury, a sunspot umbra, and the aureole. The direct observations result in Mercury intensities < 0.06 I⊙ and aureole intensities <0.01 I⊙. The stray light correction to the spot intensities has been <(0.03 ± 0.01) I⊙. The main contribution to the stray light on the solar disc is shown to be produced by a spread-function with a half width of 10 arc sec. Consequently, for stray light corrections the range R ⩽ R⊙ + + 20″ in the aureole has to be measured very precisely; furthermore, a remarkable fraction of the stray light in the center of an umbra originates from the surrounding penumbra. © D. Reidel Publishing Company 1971 |
| abstractGer |
Abstract In order to test the usual method for correcting sunspot intensity measurements for stray light, we have measured, during the Mercury transit of 1970 May 9, the intensities of Mercury, a sunspot umbra, and the aureole. The direct observations result in Mercury intensities < 0.06 I⊙ and aureole intensities <0.01 I⊙. The stray light correction to the spot intensities has been <(0.03 ± 0.01) I⊙. The main contribution to the stray light on the solar disc is shown to be produced by a spread-function with a half width of 10 arc sec. Consequently, for stray light corrections the range R ⩽ R⊙ + + 20″ in the aureole has to be measured very precisely; furthermore, a remarkable fraction of the stray light in the center of an umbra originates from the surrounding penumbra. © D. Reidel Publishing Company 1971 |
| abstract_unstemmed |
Abstract In order to test the usual method for correcting sunspot intensity measurements for stray light, we have measured, during the Mercury transit of 1970 May 9, the intensities of Mercury, a sunspot umbra, and the aureole. The direct observations result in Mercury intensities < 0.06 I⊙ and aureole intensities <0.01 I⊙. The stray light correction to the spot intensities has been <(0.03 ± 0.01) I⊙. The main contribution to the stray light on the solar disc is shown to be produced by a spread-function with a half width of 10 arc sec. Consequently, for stray light corrections the range R ⩽ R⊙ + + 20″ in the aureole has to be measured very precisely; furthermore, a remarkable fraction of the stray light in the center of an umbra originates from the surrounding penumbra. © D. Reidel Publishing Company 1971 |
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3 |
| title_short |
Observations of stray-light and sunspot intensities during the Mercury transit of 1970 May 9 |
| url |
https://doi.org/10.1007/BF00149065 |
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| up_date |
2024-07-03T17:19:42.911Z |
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