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...
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| Autor*in: |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
1971 |
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| Umfang: |
9 |
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| Reproduktion: |
Springer Online Journal Archives 1860-2002 |
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| Übergeordnetes Werk: |
in: Solar physics - 1967, 18(1971) vom: März, Seite 434-442 |
| Übergeordnetes Werk: |
volume:18 ; year:1971 ; month:03 ; pages:434-442 ; extent:9 |
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NLEJ195865766 |
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| 245 | 1 | 0 | |a Observations of stray-light and sunspot intensities during the Mercury transit of 1970 May 9 |
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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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(DE-627)NLEJ195865766 DE-627 ger DE-627 rakwb eng Observations of stray-light and sunspot intensities during the Mercury transit of 1970 May 9 1971 9 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier 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. Springer Online Journal Archives 1860-2002 Mattig, W. oth in Solar physics 1967 18(1971) vom: März, Seite 434-442 (DE-627)NLEJ188983465 (DE-600)1473830-2 1573-093X nnns volume:18 year:1971 month:03 pages:434-442 extent:9 http://dx.doi.org/10.1007/BF00149065 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 18 1971 3 434-442 9 |
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(DE-627)NLEJ195865766 DE-627 ger DE-627 rakwb eng Observations of stray-light and sunspot intensities during the Mercury transit of 1970 May 9 1971 9 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier 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. Springer Online Journal Archives 1860-2002 Mattig, W. oth in Solar physics 1967 18(1971) vom: März, Seite 434-442 (DE-627)NLEJ188983465 (DE-600)1473830-2 1573-093X nnns volume:18 year:1971 month:03 pages:434-442 extent:9 http://dx.doi.org/10.1007/BF00149065 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 18 1971 3 434-442 9 |
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(DE-627)NLEJ195865766 DE-627 ger DE-627 rakwb eng Observations of stray-light and sunspot intensities during the Mercury transit of 1970 May 9 1971 9 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier 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. Springer Online Journal Archives 1860-2002 Mattig, W. oth in Solar physics 1967 18(1971) vom: März, Seite 434-442 (DE-627)NLEJ188983465 (DE-600)1473830-2 1573-093X nnns volume:18 year:1971 month:03 pages:434-442 extent:9 http://dx.doi.org/10.1007/BF00149065 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 18 1971 3 434-442 9 |
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(DE-627)NLEJ195865766 DE-627 ger DE-627 rakwb eng Observations of stray-light and sunspot intensities during the Mercury transit of 1970 May 9 1971 9 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier 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. Springer Online Journal Archives 1860-2002 Mattig, W. oth in Solar physics 1967 18(1971) vom: März, Seite 434-442 (DE-627)NLEJ188983465 (DE-600)1473830-2 1573-093X nnns volume:18 year:1971 month:03 pages:434-442 extent:9 http://dx.doi.org/10.1007/BF00149065 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 18 1971 3 434-442 9 |
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(DE-627)NLEJ195865766 DE-627 ger DE-627 rakwb eng Observations of stray-light and sunspot intensities during the Mercury transit of 1970 May 9 1971 9 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier 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. Springer Online Journal Archives 1860-2002 Mattig, W. oth in Solar physics 1967 18(1971) vom: März, Seite 434-442 (DE-627)NLEJ188983465 (DE-600)1473830-2 1573-093X nnns volume:18 year:1971 month:03 pages:434-442 extent:9 http://dx.doi.org/10.1007/BF00149065 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 18 1971 3 434-442 9 |
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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 |
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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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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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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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