Interpretation of Solar Magnetic Field Strength Observations
Abstract This study based on longitudinal Zeeman effect magnetograms and spectral line scans investigates the dependence of solar surface magnetic fields on the spectral line used and the way the line is sampled to estimate the magnetic flux emerging above the solar atmosphere and penetrating to the...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Ulrich, R. K. [verfasserIn] |
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| Format: |
Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2009 |
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| Schlagwörter: |
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| Anmerkung: |
© The Author(s) 2009 |
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| Übergeordnetes Werk: |
Enthalten in: Solar physics - Springer Netherlands, 1967, 255(2009), 1 vom: 15. Jan., Seite 53-78 |
|---|---|
| Übergeordnetes Werk: |
volume:255 ; year:2009 ; number:1 ; day:15 ; month:01 ; pages:53-78 |
| Links: |
|---|
| DOI / URN: |
10.1007/s11207-008-9302-9 |
|---|
| Katalog-ID: |
OLC2033605361 |
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| 100 | 1 | |a Ulrich, R. K. |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a Interpretation of Solar Magnetic Field Strength Observations |
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| 520 | |a Abstract This study based on longitudinal Zeeman effect magnetograms and spectral line scans investigates the dependence of solar surface magnetic fields on the spectral line used and the way the line is sampled to estimate the magnetic flux emerging above the solar atmosphere and penetrating to the corona from magnetograms of the Mt. Wilson 150-foot tower synoptic program (MWO). We have compared the synoptic program λ5250 Å line of Fe i to the line of Fe i at λ5233 Å since this latter line has a broad shape with a profile that is nearly linear over a large portion of its wings. The present study uses five pairs of sampling points on the λ5233 Å line. Line profile observations show that the determination of the field strength from the Stokes V parameter or from line bisectors in the circularly polarized line profiles lead to similar dependencies on the spectral sampling of the lines, with the bisector method being the less sensitive. We recommend adoption of the field determined with the line bisector method as the best estimate of the emergent photospheric flux and further recommend the use of a sampling point as close to the line core as is practical. The combination of the line profile measurements and the cross-correlation of fields measured simultaneously with λ5250 Å and λ5233 Å yields a formula for the scale factor δ−1 that multiplies the MWO synoptic magnetic fields. By using ρ as the center-to-limb angle (CLA), a fit to this scale factor is δ−1=4.15−2.82sin 2(ρ). Previously δ−1=4.5−2.5sin 2(ρ) had been used. The new calibration shows that magnetic fields measured by the MDI system on the SOHO spacecraft are equal to 0.619±0.018 times the true value at a center-to-limb position 30°. Berger and Lites (2003, Solar Phys.213, 213) found this factor to be 0.64±0.013 based on a comparison using the Advanced Stokes Polarimeter. | ||
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| 700 | 1 | |a Boyden, J. E. |4 aut | |
| 700 | 1 | |a Webster, L. |4 aut | |
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10.1007/s11207-008-9302-9 doi (DE-627)OLC2033605361 (DE-He213)s11207-008-9302-9-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Ulrich, R. K. verfasserin aut Interpretation of Solar Magnetic Field Strength Observations 2009 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © The Author(s) 2009 Abstract This study based on longitudinal Zeeman effect magnetograms and spectral line scans investigates the dependence of solar surface magnetic fields on the spectral line used and the way the line is sampled to estimate the magnetic flux emerging above the solar atmosphere and penetrating to the corona from magnetograms of the Mt. Wilson 150-foot tower synoptic program (MWO). We have compared the synoptic program λ5250 Å line of Fe i to the line of Fe i at λ5233 Å since this latter line has a broad shape with a profile that is nearly linear over a large portion of its wings. The present study uses five pairs of sampling points on the λ5233 Å line. Line profile observations show that the determination of the field strength from the Stokes V parameter or from line bisectors in the circularly polarized line profiles lead to similar dependencies on the spectral sampling of the lines, with the bisector method being the less sensitive. We recommend adoption of the field determined with the line bisector method as the best estimate of the emergent photospheric flux and further recommend the use of a sampling point as close to the line core as is practical. The combination of the line profile measurements and the cross-correlation of fields measured simultaneously with λ5250 Å and λ5233 Å yields a formula for the scale factor δ−1 that multiplies the MWO synoptic magnetic fields. By using ρ as the center-to-limb angle (CLA), a fit to this scale factor is δ−1=4.15−2.82sin 2(ρ). Previously δ−1=4.5−2.5sin 2(ρ) had been used. The new calibration shows that magnetic fields measured by the MDI system on the SOHO spacecraft are equal to 0.619±0.018 times the true value at a center-to-limb position 30°. Berger and Lites (2003, Solar Phys.213, 213) found this factor to be 0.64±0.013 based on a comparison using the Advanced Stokes Polarimeter. Chromosphere, active Magnetic fields, chromosphere Magnetic fields, photosphere Bertello, L. aut Boyden, J. E. aut Webster, L. aut Enthalten in Solar physics Springer Netherlands, 1967 255(2009), 1 vom: 15. Jan., Seite 53-78 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:255 year:2009 number:1 day:15 month:01 pages:53-78 https://doi.org/10.1007/s11207-008-9302-9 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 AR 255 2009 1 15 01 53-78 |
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10.1007/s11207-008-9302-9 doi (DE-627)OLC2033605361 (DE-He213)s11207-008-9302-9-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Ulrich, R. K. verfasserin aut Interpretation of Solar Magnetic Field Strength Observations 2009 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © The Author(s) 2009 Abstract This study based on longitudinal Zeeman effect magnetograms and spectral line scans investigates the dependence of solar surface magnetic fields on the spectral line used and the way the line is sampled to estimate the magnetic flux emerging above the solar atmosphere and penetrating to the corona from magnetograms of the Mt. Wilson 150-foot tower synoptic program (MWO). We have compared the synoptic program λ5250 Å line of Fe i to the line of Fe i at λ5233 Å since this latter line has a broad shape with a profile that is nearly linear over a large portion of its wings. The present study uses five pairs of sampling points on the λ5233 Å line. Line profile observations show that the determination of the field strength from the Stokes V parameter or from line bisectors in the circularly polarized line profiles lead to similar dependencies on the spectral sampling of the lines, with the bisector method being the less sensitive. We recommend adoption of the field determined with the line bisector method as the best estimate of the emergent photospheric flux and further recommend the use of a sampling point as close to the line core as is practical. The combination of the line profile measurements and the cross-correlation of fields measured simultaneously with λ5250 Å and λ5233 Å yields a formula for the scale factor δ−1 that multiplies the MWO synoptic magnetic fields. By using ρ as the center-to-limb angle (CLA), a fit to this scale factor is δ−1=4.15−2.82sin 2(ρ). Previously δ−1=4.5−2.5sin 2(ρ) had been used. The new calibration shows that magnetic fields measured by the MDI system on the SOHO spacecraft are equal to 0.619±0.018 times the true value at a center-to-limb position 30°. Berger and Lites (2003, Solar Phys.213, 213) found this factor to be 0.64±0.013 based on a comparison using the Advanced Stokes Polarimeter. Chromosphere, active Magnetic fields, chromosphere Magnetic fields, photosphere Bertello, L. aut Boyden, J. E. aut Webster, L. aut Enthalten in Solar physics Springer Netherlands, 1967 255(2009), 1 vom: 15. Jan., Seite 53-78 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:255 year:2009 number:1 day:15 month:01 pages:53-78 https://doi.org/10.1007/s11207-008-9302-9 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 AR 255 2009 1 15 01 53-78 |
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10.1007/s11207-008-9302-9 doi (DE-627)OLC2033605361 (DE-He213)s11207-008-9302-9-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Ulrich, R. K. verfasserin aut Interpretation of Solar Magnetic Field Strength Observations 2009 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © The Author(s) 2009 Abstract This study based on longitudinal Zeeman effect magnetograms and spectral line scans investigates the dependence of solar surface magnetic fields on the spectral line used and the way the line is sampled to estimate the magnetic flux emerging above the solar atmosphere and penetrating to the corona from magnetograms of the Mt. Wilson 150-foot tower synoptic program (MWO). We have compared the synoptic program λ5250 Å line of Fe i to the line of Fe i at λ5233 Å since this latter line has a broad shape with a profile that is nearly linear over a large portion of its wings. The present study uses five pairs of sampling points on the λ5233 Å line. Line profile observations show that the determination of the field strength from the Stokes V parameter or from line bisectors in the circularly polarized line profiles lead to similar dependencies on the spectral sampling of the lines, with the bisector method being the less sensitive. We recommend adoption of the field determined with the line bisector method as the best estimate of the emergent photospheric flux and further recommend the use of a sampling point as close to the line core as is practical. The combination of the line profile measurements and the cross-correlation of fields measured simultaneously with λ5250 Å and λ5233 Å yields a formula for the scale factor δ−1 that multiplies the MWO synoptic magnetic fields. By using ρ as the center-to-limb angle (CLA), a fit to this scale factor is δ−1=4.15−2.82sin 2(ρ). Previously δ−1=4.5−2.5sin 2(ρ) had been used. The new calibration shows that magnetic fields measured by the MDI system on the SOHO spacecraft are equal to 0.619±0.018 times the true value at a center-to-limb position 30°. Berger and Lites (2003, Solar Phys.213, 213) found this factor to be 0.64±0.013 based on a comparison using the Advanced Stokes Polarimeter. Chromosphere, active Magnetic fields, chromosphere Magnetic fields, photosphere Bertello, L. aut Boyden, J. E. aut Webster, L. aut Enthalten in Solar physics Springer Netherlands, 1967 255(2009), 1 vom: 15. Jan., Seite 53-78 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:255 year:2009 number:1 day:15 month:01 pages:53-78 https://doi.org/10.1007/s11207-008-9302-9 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 AR 255 2009 1 15 01 53-78 |
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10.1007/s11207-008-9302-9 doi (DE-627)OLC2033605361 (DE-He213)s11207-008-9302-9-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Ulrich, R. K. verfasserin aut Interpretation of Solar Magnetic Field Strength Observations 2009 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © The Author(s) 2009 Abstract This study based on longitudinal Zeeman effect magnetograms and spectral line scans investigates the dependence of solar surface magnetic fields on the spectral line used and the way the line is sampled to estimate the magnetic flux emerging above the solar atmosphere and penetrating to the corona from magnetograms of the Mt. Wilson 150-foot tower synoptic program (MWO). We have compared the synoptic program λ5250 Å line of Fe i to the line of Fe i at λ5233 Å since this latter line has a broad shape with a profile that is nearly linear over a large portion of its wings. The present study uses five pairs of sampling points on the λ5233 Å line. Line profile observations show that the determination of the field strength from the Stokes V parameter or from line bisectors in the circularly polarized line profiles lead to similar dependencies on the spectral sampling of the lines, with the bisector method being the less sensitive. We recommend adoption of the field determined with the line bisector method as the best estimate of the emergent photospheric flux and further recommend the use of a sampling point as close to the line core as is practical. The combination of the line profile measurements and the cross-correlation of fields measured simultaneously with λ5250 Å and λ5233 Å yields a formula for the scale factor δ−1 that multiplies the MWO synoptic magnetic fields. By using ρ as the center-to-limb angle (CLA), a fit to this scale factor is δ−1=4.15−2.82sin 2(ρ). Previously δ−1=4.5−2.5sin 2(ρ) had been used. The new calibration shows that magnetic fields measured by the MDI system on the SOHO spacecraft are equal to 0.619±0.018 times the true value at a center-to-limb position 30°. Berger and Lites (2003, Solar Phys.213, 213) found this factor to be 0.64±0.013 based on a comparison using the Advanced Stokes Polarimeter. Chromosphere, active Magnetic fields, chromosphere Magnetic fields, photosphere Bertello, L. aut Boyden, J. E. aut Webster, L. aut Enthalten in Solar physics Springer Netherlands, 1967 255(2009), 1 vom: 15. Jan., Seite 53-78 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:255 year:2009 number:1 day:15 month:01 pages:53-78 https://doi.org/10.1007/s11207-008-9302-9 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 AR 255 2009 1 15 01 53-78 |
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10.1007/s11207-008-9302-9 doi (DE-627)OLC2033605361 (DE-He213)s11207-008-9302-9-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Ulrich, R. K. verfasserin aut Interpretation of Solar Magnetic Field Strength Observations 2009 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © The Author(s) 2009 Abstract This study based on longitudinal Zeeman effect magnetograms and spectral line scans investigates the dependence of solar surface magnetic fields on the spectral line used and the way the line is sampled to estimate the magnetic flux emerging above the solar atmosphere and penetrating to the corona from magnetograms of the Mt. Wilson 150-foot tower synoptic program (MWO). We have compared the synoptic program λ5250 Å line of Fe i to the line of Fe i at λ5233 Å since this latter line has a broad shape with a profile that is nearly linear over a large portion of its wings. The present study uses five pairs of sampling points on the λ5233 Å line. Line profile observations show that the determination of the field strength from the Stokes V parameter or from line bisectors in the circularly polarized line profiles lead to similar dependencies on the spectral sampling of the lines, with the bisector method being the less sensitive. We recommend adoption of the field determined with the line bisector method as the best estimate of the emergent photospheric flux and further recommend the use of a sampling point as close to the line core as is practical. The combination of the line profile measurements and the cross-correlation of fields measured simultaneously with λ5250 Å and λ5233 Å yields a formula for the scale factor δ−1 that multiplies the MWO synoptic magnetic fields. By using ρ as the center-to-limb angle (CLA), a fit to this scale factor is δ−1=4.15−2.82sin 2(ρ). Previously δ−1=4.5−2.5sin 2(ρ) had been used. The new calibration shows that magnetic fields measured by the MDI system on the SOHO spacecraft are equal to 0.619±0.018 times the true value at a center-to-limb position 30°. Berger and Lites (2003, Solar Phys.213, 213) found this factor to be 0.64±0.013 based on a comparison using the Advanced Stokes Polarimeter. Chromosphere, active Magnetic fields, chromosphere Magnetic fields, photosphere Bertello, L. aut Boyden, J. E. aut Webster, L. aut Enthalten in Solar physics Springer Netherlands, 1967 255(2009), 1 vom: 15. Jan., Seite 53-78 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:255 year:2009 number:1 day:15 month:01 pages:53-78 https://doi.org/10.1007/s11207-008-9302-9 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 AR 255 2009 1 15 01 53-78 |
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| author |
Ulrich, R. K. |
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Ulrich, R. K. ddc 530 ssgn 16,12 misc Chromosphere, active misc Magnetic fields, chromosphere misc Magnetic fields, photosphere Interpretation of Solar Magnetic Field Strength Observations |
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530 VZ 16,12 ssgn Interpretation of Solar Magnetic Field Strength Observations Chromosphere, active Magnetic fields, chromosphere Magnetic fields, photosphere |
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ddc 530 ssgn 16,12 misc Chromosphere, active misc Magnetic fields, chromosphere misc Magnetic fields, photosphere |
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Interpretation of Solar Magnetic Field Strength Observations |
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Interpretation of Solar Magnetic Field Strength Observations |
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Ulrich, R. K. |
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Solar physics |
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Ulrich, R. K. Bertello, L. Boyden, J. E. Webster, L. |
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Ulrich, R. K. |
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10.1007/s11207-008-9302-9 |
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530 |
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interpretation of solar magnetic field strength observations |
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Interpretation of Solar Magnetic Field Strength Observations |
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Abstract This study based on longitudinal Zeeman effect magnetograms and spectral line scans investigates the dependence of solar surface magnetic fields on the spectral line used and the way the line is sampled to estimate the magnetic flux emerging above the solar atmosphere and penetrating to the corona from magnetograms of the Mt. Wilson 150-foot tower synoptic program (MWO). We have compared the synoptic program λ5250 Å line of Fe i to the line of Fe i at λ5233 Å since this latter line has a broad shape with a profile that is nearly linear over a large portion of its wings. The present study uses five pairs of sampling points on the λ5233 Å line. Line profile observations show that the determination of the field strength from the Stokes V parameter or from line bisectors in the circularly polarized line profiles lead to similar dependencies on the spectral sampling of the lines, with the bisector method being the less sensitive. We recommend adoption of the field determined with the line bisector method as the best estimate of the emergent photospheric flux and further recommend the use of a sampling point as close to the line core as is practical. The combination of the line profile measurements and the cross-correlation of fields measured simultaneously with λ5250 Å and λ5233 Å yields a formula for the scale factor δ−1 that multiplies the MWO synoptic magnetic fields. By using ρ as the center-to-limb angle (CLA), a fit to this scale factor is δ−1=4.15−2.82sin 2(ρ). Previously δ−1=4.5−2.5sin 2(ρ) had been used. The new calibration shows that magnetic fields measured by the MDI system on the SOHO spacecraft are equal to 0.619±0.018 times the true value at a center-to-limb position 30°. Berger and Lites (2003, Solar Phys.213, 213) found this factor to be 0.64±0.013 based on a comparison using the Advanced Stokes Polarimeter. © The Author(s) 2009 |
| abstractGer |
Abstract This study based on longitudinal Zeeman effect magnetograms and spectral line scans investigates the dependence of solar surface magnetic fields on the spectral line used and the way the line is sampled to estimate the magnetic flux emerging above the solar atmosphere and penetrating to the corona from magnetograms of the Mt. Wilson 150-foot tower synoptic program (MWO). We have compared the synoptic program λ5250 Å line of Fe i to the line of Fe i at λ5233 Å since this latter line has a broad shape with a profile that is nearly linear over a large portion of its wings. The present study uses five pairs of sampling points on the λ5233 Å line. Line profile observations show that the determination of the field strength from the Stokes V parameter or from line bisectors in the circularly polarized line profiles lead to similar dependencies on the spectral sampling of the lines, with the bisector method being the less sensitive. We recommend adoption of the field determined with the line bisector method as the best estimate of the emergent photospheric flux and further recommend the use of a sampling point as close to the line core as is practical. The combination of the line profile measurements and the cross-correlation of fields measured simultaneously with λ5250 Å and λ5233 Å yields a formula for the scale factor δ−1 that multiplies the MWO synoptic magnetic fields. By using ρ as the center-to-limb angle (CLA), a fit to this scale factor is δ−1=4.15−2.82sin 2(ρ). Previously δ−1=4.5−2.5sin 2(ρ) had been used. The new calibration shows that magnetic fields measured by the MDI system on the SOHO spacecraft are equal to 0.619±0.018 times the true value at a center-to-limb position 30°. Berger and Lites (2003, Solar Phys.213, 213) found this factor to be 0.64±0.013 based on a comparison using the Advanced Stokes Polarimeter. © The Author(s) 2009 |
| abstract_unstemmed |
Abstract This study based on longitudinal Zeeman effect magnetograms and spectral line scans investigates the dependence of solar surface magnetic fields on the spectral line used and the way the line is sampled to estimate the magnetic flux emerging above the solar atmosphere and penetrating to the corona from magnetograms of the Mt. Wilson 150-foot tower synoptic program (MWO). We have compared the synoptic program λ5250 Å line of Fe i to the line of Fe i at λ5233 Å since this latter line has a broad shape with a profile that is nearly linear over a large portion of its wings. The present study uses five pairs of sampling points on the λ5233 Å line. Line profile observations show that the determination of the field strength from the Stokes V parameter or from line bisectors in the circularly polarized line profiles lead to similar dependencies on the spectral sampling of the lines, with the bisector method being the less sensitive. We recommend adoption of the field determined with the line bisector method as the best estimate of the emergent photospheric flux and further recommend the use of a sampling point as close to the line core as is practical. The combination of the line profile measurements and the cross-correlation of fields measured simultaneously with λ5250 Å and λ5233 Å yields a formula for the scale factor δ−1 that multiplies the MWO synoptic magnetic fields. By using ρ as the center-to-limb angle (CLA), a fit to this scale factor is δ−1=4.15−2.82sin 2(ρ). Previously δ−1=4.5−2.5sin 2(ρ) had been used. The new calibration shows that magnetic fields measured by the MDI system on the SOHO spacecraft are equal to 0.619±0.018 times the true value at a center-to-limb position 30°. Berger and Lites (2003, Solar Phys.213, 213) found this factor to be 0.64±0.013 based on a comparison using the Advanced Stokes Polarimeter. © The Author(s) 2009 |
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Interpretation of Solar Magnetic Field Strength Observations |
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