Complete determination of the magnetic field vector and of the electron density in 14 prominences from linear polarizaton measurements in the HeI $ D_{3} $ and Hα lines
Abstract The present paper is devoted to the interpretation of linear polarization data obtained in 14 quiescent prominences with the Pic-du-Midi coronagraph-polarimeter by J. L. Leroy, in the two lines Hei $ D_{3} $ andHα quasi-simultaneously. The linear polarization of the lines is due to scatteri...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Bommier, Véronique [verfasserIn] |
|---|
| Format: |
Artikel |
|---|---|
| Sprache: |
Englisch |
| Erschienen: |
1994 |
|---|
| Schlagwörter: |
|---|
| Anmerkung: |
© Kluwer Academic Publishers 1994 |
|---|
| Übergeordnetes Werk: |
Enthalten in: Solar physics - Kluwer Academic Publishers, 1967, 154(1994), 2 vom: Okt., Seite 231-260 |
|---|---|
| Übergeordnetes Werk: |
volume:154 ; year:1994 ; number:2 ; month:10 ; pages:231-260 |
| Links: |
|---|
| DOI / URN: |
10.1007/BF00681098 |
|---|
| Katalog-ID: |
OLC2033576558 |
|---|
| LEADER | 01000caa a22002652 4500 | ||
|---|---|---|---|
| 001 | OLC2033576558 | ||
| 003 | DE-627 | ||
| 005 | 20230504045555.0 | ||
| 007 | tu | ||
| 008 | 200819s1994 xx ||||| 00| ||eng c | ||
| 024 | 7 | |a 10.1007/BF00681098 |2 doi | |
| 035 | |a (DE-627)OLC2033576558 | ||
| 035 | |a (DE-He213)BF00681098-p | ||
| 040 | |a DE-627 |b ger |c DE-627 |e rakwb | ||
| 041 | |a eng | ||
| 082 | 0 | 4 | |a 530 |q VZ |
| 084 | |a 16,12 |2 ssgn | ||
| 100 | 1 | |a Bommier, Véronique |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a Complete determination of the magnetic field vector and of the electron density in 14 prominences from linear polarizaton measurements in the HeI $ D_{3} $ and Hα lines |
| 264 | 1 | |c 1994 | |
| 336 | |a Text |b txt |2 rdacontent | ||
| 337 | |a ohne Hilfsmittel zu benutzen |b n |2 rdamedia | ||
| 338 | |a Band |b nc |2 rdacarrier | ||
| 500 | |a © Kluwer Academic Publishers 1994 | ||
| 520 | |a Abstract The present paper is devoted to the interpretation of linear polarization data obtained in 14 quiescent prominences with the Pic-du-Midi coronagraph-polarimeter by J. L. Leroy, in the two lines Hei $ D_{3} $ andHα quasi-simultaneously. The linear polarization of the lines is due to scattering of the anisotropic photospheric radiation, modified by the Hanle effect due to the local magnetic field. The interpretation of the polarization data in the two lines is able to provide the 3 components of the magnetic field vector, and one extra parameter, namely the electron density, because the linear polarization of Hα is also sensitive to the depolarizing effect of collisions with the electrons and protons of the medium. Moreover, by using two lines with different optical thicknesses, namely Hei $ D_{3} $, which is optically thin, and Hα, which is optically thick (τ = 1), it is possible to solve the fundamental ambiguity, each line providing two field vector solutions that are symmetrical in direction with respect to the line of sight in the case of the optically thin line, and which have a different symmetry in the case of the optically thick line. It is then possible to determine without ambiguity the polarity of the prominence magnetic field with respect to that of the photospheric field: 12 prominences are found to be Inverse polarity prominences, whereas 2 prominences are found to be Normal polarity prominences. It must be noticed that in 12 of the 14 cases, the line-of-sight component of the magnetic field vector has a Normal polarity (to the extent that the notion of polarity of a vector component is meaningful; no polarity can be derived in the 2 remaining cases); this may explain the controversy between the results obtained with methods based on the Hanle effect with results obtained through the Zeeman effect. A dip of the magnetic field lines across the prominence has been assumed, to which the optically thick Hα line is sensitive, and the optically thin Hei $ D_{3} $ line is insensitive. For the Inverse prominences, the average field strength is 7.5±1.2 G, the average angle,α, between the field vector and the prominence long axis is 36° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 29° ± 20°, and the average electron density is 2.1 × $ 10^{10} $ ± 0.7 × $ 10^{10} $ $ cm^{−3} $. For the Normal prominences, the average field strength is 13.2±2.0 G, the average angle,α, between the field vector and the prominence long axis is 53° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 0° ± 20° (horizontal field), and the average electron density is 8.7 × $ 10^{9} $ ± 3.0 × $ 10^{9} $ $ cm^{−3} $. | ||
| 650 | 4 | |a Field Vector | |
| 650 | 4 | |a Linear Polarization | |
| 650 | 4 | |a Polarization Data | |
| 650 | 4 | |a Solar Surface | |
| 650 | 4 | |a Normal Polarity | |
| 700 | 1 | |a Degl'Innocenti, Egidio Landi |4 aut | |
| 700 | 1 | |a Leroy, Jean-Louis |4 aut | |
| 700 | 1 | |a Sahal-Bréchot, Sylvie |4 aut | |
| 773 | 0 | 8 | |i Enthalten in |t Solar physics |d Kluwer Academic Publishers, 1967 |g 154(1994), 2 vom: Okt., Seite 231-260 |w (DE-627)129856010 |w (DE-600)281593-X |w (DE-576)015160033 |x 0038-0938 |7 nnns |
| 773 | 1 | 8 | |g volume:154 |g year:1994 |g number:2 |g month:10 |g pages:231-260 |
| 856 | 4 | 1 | |u https://doi.org/10.1007/BF00681098 |z lizenzpflichtig |3 Volltext |
| 912 | |a GBV_USEFLAG_A | ||
| 912 | |a SYSFLAG_A | ||
| 912 | |a GBV_OLC | ||
| 912 | |a SSG-OLC-PHY | ||
| 912 | |a SSG-OLC-AST | ||
| 912 | |a SSG-OPC-AST | ||
| 912 | |a GBV_ILN_11 | ||
| 912 | |a GBV_ILN_22 | ||
| 912 | |a GBV_ILN_40 | ||
| 912 | |a GBV_ILN_47 | ||
| 912 | |a GBV_ILN_70 | ||
| 912 | |a GBV_ILN_2002 | ||
| 912 | |a GBV_ILN_2279 | ||
| 912 | |a GBV_ILN_2286 | ||
| 912 | |a GBV_ILN_4012 | ||
| 912 | |a GBV_ILN_4306 | ||
| 951 | |a AR | ||
| 952 | |d 154 |j 1994 |e 2 |c 10 |h 231-260 | ||
| author_variant |
v b vb e l d el eld j l l jll s s b ssb |
|---|---|
| matchkey_str |
article:00380938:1994----::opeeeemntooteantcilvcoadfheetodniyn4rmnnefolnaplrzt |
| hierarchy_sort_str |
1994 |
| publishDate |
1994 |
| allfields |
10.1007/BF00681098 doi (DE-627)OLC2033576558 (DE-He213)BF00681098-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Bommier, Véronique verfasserin aut Complete determination of the magnetic field vector and of the electron density in 14 prominences from linear polarizaton measurements in the HeI $ D_{3} $ and Hα lines 1994 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1994 Abstract The present paper is devoted to the interpretation of linear polarization data obtained in 14 quiescent prominences with the Pic-du-Midi coronagraph-polarimeter by J. L. Leroy, in the two lines Hei $ D_{3} $ andHα quasi-simultaneously. The linear polarization of the lines is due to scattering of the anisotropic photospheric radiation, modified by the Hanle effect due to the local magnetic field. The interpretation of the polarization data in the two lines is able to provide the 3 components of the magnetic field vector, and one extra parameter, namely the electron density, because the linear polarization of Hα is also sensitive to the depolarizing effect of collisions with the electrons and protons of the medium. Moreover, by using two lines with different optical thicknesses, namely Hei $ D_{3} $, which is optically thin, and Hα, which is optically thick (τ = 1), it is possible to solve the fundamental ambiguity, each line providing two field vector solutions that are symmetrical in direction with respect to the line of sight in the case of the optically thin line, and which have a different symmetry in the case of the optically thick line. It is then possible to determine without ambiguity the polarity of the prominence magnetic field with respect to that of the photospheric field: 12 prominences are found to be Inverse polarity prominences, whereas 2 prominences are found to be Normal polarity prominences. It must be noticed that in 12 of the 14 cases, the line-of-sight component of the magnetic field vector has a Normal polarity (to the extent that the notion of polarity of a vector component is meaningful; no polarity can be derived in the 2 remaining cases); this may explain the controversy between the results obtained with methods based on the Hanle effect with results obtained through the Zeeman effect. A dip of the magnetic field lines across the prominence has been assumed, to which the optically thick Hα line is sensitive, and the optically thin Hei $ D_{3} $ line is insensitive. For the Inverse prominences, the average field strength is 7.5±1.2 G, the average angle,α, between the field vector and the prominence long axis is 36° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 29° ± 20°, and the average electron density is 2.1 × $ 10^{10} $ ± 0.7 × $ 10^{10} $ $ cm^{−3} $. For the Normal prominences, the average field strength is 13.2±2.0 G, the average angle,α, between the field vector and the prominence long axis is 53° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 0° ± 20° (horizontal field), and the average electron density is 8.7 × $ 10^{9} $ ± 3.0 × $ 10^{9} $ $ cm^{−3} $. Field Vector Linear Polarization Polarization Data Solar Surface Normal Polarity Degl'Innocenti, Egidio Landi aut Leroy, Jean-Louis aut Sahal-Bréchot, Sylvie aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 154(1994), 2 vom: Okt., Seite 231-260 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:154 year:1994 number:2 month:10 pages:231-260 https://doi.org/10.1007/BF00681098 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4306 AR 154 1994 2 10 231-260 |
| spelling |
10.1007/BF00681098 doi (DE-627)OLC2033576558 (DE-He213)BF00681098-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Bommier, Véronique verfasserin aut Complete determination of the magnetic field vector and of the electron density in 14 prominences from linear polarizaton measurements in the HeI $ D_{3} $ and Hα lines 1994 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1994 Abstract The present paper is devoted to the interpretation of linear polarization data obtained in 14 quiescent prominences with the Pic-du-Midi coronagraph-polarimeter by J. L. Leroy, in the two lines Hei $ D_{3} $ andHα quasi-simultaneously. The linear polarization of the lines is due to scattering of the anisotropic photospheric radiation, modified by the Hanle effect due to the local magnetic field. The interpretation of the polarization data in the two lines is able to provide the 3 components of the magnetic field vector, and one extra parameter, namely the electron density, because the linear polarization of Hα is also sensitive to the depolarizing effect of collisions with the electrons and protons of the medium. Moreover, by using two lines with different optical thicknesses, namely Hei $ D_{3} $, which is optically thin, and Hα, which is optically thick (τ = 1), it is possible to solve the fundamental ambiguity, each line providing two field vector solutions that are symmetrical in direction with respect to the line of sight in the case of the optically thin line, and which have a different symmetry in the case of the optically thick line. It is then possible to determine without ambiguity the polarity of the prominence magnetic field with respect to that of the photospheric field: 12 prominences are found to be Inverse polarity prominences, whereas 2 prominences are found to be Normal polarity prominences. It must be noticed that in 12 of the 14 cases, the line-of-sight component of the magnetic field vector has a Normal polarity (to the extent that the notion of polarity of a vector component is meaningful; no polarity can be derived in the 2 remaining cases); this may explain the controversy between the results obtained with methods based on the Hanle effect with results obtained through the Zeeman effect. A dip of the magnetic field lines across the prominence has been assumed, to which the optically thick Hα line is sensitive, and the optically thin Hei $ D_{3} $ line is insensitive. For the Inverse prominences, the average field strength is 7.5±1.2 G, the average angle,α, between the field vector and the prominence long axis is 36° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 29° ± 20°, and the average electron density is 2.1 × $ 10^{10} $ ± 0.7 × $ 10^{10} $ $ cm^{−3} $. For the Normal prominences, the average field strength is 13.2±2.0 G, the average angle,α, between the field vector and the prominence long axis is 53° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 0° ± 20° (horizontal field), and the average electron density is 8.7 × $ 10^{9} $ ± 3.0 × $ 10^{9} $ $ cm^{−3} $. Field Vector Linear Polarization Polarization Data Solar Surface Normal Polarity Degl'Innocenti, Egidio Landi aut Leroy, Jean-Louis aut Sahal-Bréchot, Sylvie aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 154(1994), 2 vom: Okt., Seite 231-260 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:154 year:1994 number:2 month:10 pages:231-260 https://doi.org/10.1007/BF00681098 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4306 AR 154 1994 2 10 231-260 |
| allfields_unstemmed |
10.1007/BF00681098 doi (DE-627)OLC2033576558 (DE-He213)BF00681098-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Bommier, Véronique verfasserin aut Complete determination of the magnetic field vector and of the electron density in 14 prominences from linear polarizaton measurements in the HeI $ D_{3} $ and Hα lines 1994 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1994 Abstract The present paper is devoted to the interpretation of linear polarization data obtained in 14 quiescent prominences with the Pic-du-Midi coronagraph-polarimeter by J. L. Leroy, in the two lines Hei $ D_{3} $ andHα quasi-simultaneously. The linear polarization of the lines is due to scattering of the anisotropic photospheric radiation, modified by the Hanle effect due to the local magnetic field. The interpretation of the polarization data in the two lines is able to provide the 3 components of the magnetic field vector, and one extra parameter, namely the electron density, because the linear polarization of Hα is also sensitive to the depolarizing effect of collisions with the electrons and protons of the medium. Moreover, by using two lines with different optical thicknesses, namely Hei $ D_{3} $, which is optically thin, and Hα, which is optically thick (τ = 1), it is possible to solve the fundamental ambiguity, each line providing two field vector solutions that are symmetrical in direction with respect to the line of sight in the case of the optically thin line, and which have a different symmetry in the case of the optically thick line. It is then possible to determine without ambiguity the polarity of the prominence magnetic field with respect to that of the photospheric field: 12 prominences are found to be Inverse polarity prominences, whereas 2 prominences are found to be Normal polarity prominences. It must be noticed that in 12 of the 14 cases, the line-of-sight component of the magnetic field vector has a Normal polarity (to the extent that the notion of polarity of a vector component is meaningful; no polarity can be derived in the 2 remaining cases); this may explain the controversy between the results obtained with methods based on the Hanle effect with results obtained through the Zeeman effect. A dip of the magnetic field lines across the prominence has been assumed, to which the optically thick Hα line is sensitive, and the optically thin Hei $ D_{3} $ line is insensitive. For the Inverse prominences, the average field strength is 7.5±1.2 G, the average angle,α, between the field vector and the prominence long axis is 36° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 29° ± 20°, and the average electron density is 2.1 × $ 10^{10} $ ± 0.7 × $ 10^{10} $ $ cm^{−3} $. For the Normal prominences, the average field strength is 13.2±2.0 G, the average angle,α, between the field vector and the prominence long axis is 53° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 0° ± 20° (horizontal field), and the average electron density is 8.7 × $ 10^{9} $ ± 3.0 × $ 10^{9} $ $ cm^{−3} $. Field Vector Linear Polarization Polarization Data Solar Surface Normal Polarity Degl'Innocenti, Egidio Landi aut Leroy, Jean-Louis aut Sahal-Bréchot, Sylvie aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 154(1994), 2 vom: Okt., Seite 231-260 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:154 year:1994 number:2 month:10 pages:231-260 https://doi.org/10.1007/BF00681098 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4306 AR 154 1994 2 10 231-260 |
| allfieldsGer |
10.1007/BF00681098 doi (DE-627)OLC2033576558 (DE-He213)BF00681098-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Bommier, Véronique verfasserin aut Complete determination of the magnetic field vector and of the electron density in 14 prominences from linear polarizaton measurements in the HeI $ D_{3} $ and Hα lines 1994 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1994 Abstract The present paper is devoted to the interpretation of linear polarization data obtained in 14 quiescent prominences with the Pic-du-Midi coronagraph-polarimeter by J. L. Leroy, in the two lines Hei $ D_{3} $ andHα quasi-simultaneously. The linear polarization of the lines is due to scattering of the anisotropic photospheric radiation, modified by the Hanle effect due to the local magnetic field. The interpretation of the polarization data in the two lines is able to provide the 3 components of the magnetic field vector, and one extra parameter, namely the electron density, because the linear polarization of Hα is also sensitive to the depolarizing effect of collisions with the electrons and protons of the medium. Moreover, by using two lines with different optical thicknesses, namely Hei $ D_{3} $, which is optically thin, and Hα, which is optically thick (τ = 1), it is possible to solve the fundamental ambiguity, each line providing two field vector solutions that are symmetrical in direction with respect to the line of sight in the case of the optically thin line, and which have a different symmetry in the case of the optically thick line. It is then possible to determine without ambiguity the polarity of the prominence magnetic field with respect to that of the photospheric field: 12 prominences are found to be Inverse polarity prominences, whereas 2 prominences are found to be Normal polarity prominences. It must be noticed that in 12 of the 14 cases, the line-of-sight component of the magnetic field vector has a Normal polarity (to the extent that the notion of polarity of a vector component is meaningful; no polarity can be derived in the 2 remaining cases); this may explain the controversy between the results obtained with methods based on the Hanle effect with results obtained through the Zeeman effect. A dip of the magnetic field lines across the prominence has been assumed, to which the optically thick Hα line is sensitive, and the optically thin Hei $ D_{3} $ line is insensitive. For the Inverse prominences, the average field strength is 7.5±1.2 G, the average angle,α, between the field vector and the prominence long axis is 36° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 29° ± 20°, and the average electron density is 2.1 × $ 10^{10} $ ± 0.7 × $ 10^{10} $ $ cm^{−3} $. For the Normal prominences, the average field strength is 13.2±2.0 G, the average angle,α, between the field vector and the prominence long axis is 53° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 0° ± 20° (horizontal field), and the average electron density is 8.7 × $ 10^{9} $ ± 3.0 × $ 10^{9} $ $ cm^{−3} $. Field Vector Linear Polarization Polarization Data Solar Surface Normal Polarity Degl'Innocenti, Egidio Landi aut Leroy, Jean-Louis aut Sahal-Bréchot, Sylvie aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 154(1994), 2 vom: Okt., Seite 231-260 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:154 year:1994 number:2 month:10 pages:231-260 https://doi.org/10.1007/BF00681098 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4306 AR 154 1994 2 10 231-260 |
| allfieldsSound |
10.1007/BF00681098 doi (DE-627)OLC2033576558 (DE-He213)BF00681098-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Bommier, Véronique verfasserin aut Complete determination of the magnetic field vector and of the electron density in 14 prominences from linear polarizaton measurements in the HeI $ D_{3} $ and Hα lines 1994 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Kluwer Academic Publishers 1994 Abstract The present paper is devoted to the interpretation of linear polarization data obtained in 14 quiescent prominences with the Pic-du-Midi coronagraph-polarimeter by J. L. Leroy, in the two lines Hei $ D_{3} $ andHα quasi-simultaneously. The linear polarization of the lines is due to scattering of the anisotropic photospheric radiation, modified by the Hanle effect due to the local magnetic field. The interpretation of the polarization data in the two lines is able to provide the 3 components of the magnetic field vector, and one extra parameter, namely the electron density, because the linear polarization of Hα is also sensitive to the depolarizing effect of collisions with the electrons and protons of the medium. Moreover, by using two lines with different optical thicknesses, namely Hei $ D_{3} $, which is optically thin, and Hα, which is optically thick (τ = 1), it is possible to solve the fundamental ambiguity, each line providing two field vector solutions that are symmetrical in direction with respect to the line of sight in the case of the optically thin line, and which have a different symmetry in the case of the optically thick line. It is then possible to determine without ambiguity the polarity of the prominence magnetic field with respect to that of the photospheric field: 12 prominences are found to be Inverse polarity prominences, whereas 2 prominences are found to be Normal polarity prominences. It must be noticed that in 12 of the 14 cases, the line-of-sight component of the magnetic field vector has a Normal polarity (to the extent that the notion of polarity of a vector component is meaningful; no polarity can be derived in the 2 remaining cases); this may explain the controversy between the results obtained with methods based on the Hanle effect with results obtained through the Zeeman effect. A dip of the magnetic field lines across the prominence has been assumed, to which the optically thick Hα line is sensitive, and the optically thin Hei $ D_{3} $ line is insensitive. For the Inverse prominences, the average field strength is 7.5±1.2 G, the average angle,α, between the field vector and the prominence long axis is 36° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 29° ± 20°, and the average electron density is 2.1 × $ 10^{10} $ ± 0.7 × $ 10^{10} $ $ cm^{−3} $. For the Normal prominences, the average field strength is 13.2±2.0 G, the average angle,α, between the field vector and the prominence long axis is 53° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 0° ± 20° (horizontal field), and the average electron density is 8.7 × $ 10^{9} $ ± 3.0 × $ 10^{9} $ $ cm^{−3} $. Field Vector Linear Polarization Polarization Data Solar Surface Normal Polarity Degl'Innocenti, Egidio Landi aut Leroy, Jean-Louis aut Sahal-Bréchot, Sylvie aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 154(1994), 2 vom: Okt., Seite 231-260 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:154 year:1994 number:2 month:10 pages:231-260 https://doi.org/10.1007/BF00681098 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4306 AR 154 1994 2 10 231-260 |
| language |
English |
| source |
Enthalten in Solar physics 154(1994), 2 vom: Okt., Seite 231-260 volume:154 year:1994 number:2 month:10 pages:231-260 |
| sourceStr |
Enthalten in Solar physics 154(1994), 2 vom: Okt., Seite 231-260 volume:154 year:1994 number:2 month:10 pages:231-260 |
| format_phy_str_mv |
Article |
| institution |
findex.gbv.de |
| topic_facet |
Field Vector Linear Polarization Polarization Data Solar Surface Normal Polarity |
| dewey-raw |
530 |
| isfreeaccess_bool |
false |
| container_title |
Solar physics |
| authorswithroles_txt_mv |
Bommier, Véronique @@aut@@ Degl'Innocenti, Egidio Landi @@aut@@ Leroy, Jean-Louis @@aut@@ Sahal-Bréchot, Sylvie @@aut@@ |
| publishDateDaySort_date |
1994-10-01T00:00:00Z |
| hierarchy_top_id |
129856010 |
| dewey-sort |
3530 |
| id |
OLC2033576558 |
| language_de |
englisch |
| fullrecord |
<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">OLC2033576558</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230504045555.0</controlfield><controlfield tag="007">tu</controlfield><controlfield tag="008">200819s1994 xx ||||| 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1007/BF00681098</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)OLC2033576558</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-He213)BF00681098-p</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">530</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">16,12</subfield><subfield code="2">ssgn</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Bommier, Véronique</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Complete determination of the magnetic field vector and of the electron density in 14 prominences from linear polarizaton measurements in the HeI $ D_{3} $ and Hα lines</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">1994</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">ohne Hilfsmittel zu benutzen</subfield><subfield code="b">n</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Band</subfield><subfield code="b">nc</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="500" ind1=" " ind2=" "><subfield code="a">© Kluwer Academic Publishers 1994</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract The present paper is devoted to the interpretation of linear polarization data obtained in 14 quiescent prominences with the Pic-du-Midi coronagraph-polarimeter by J. L. Leroy, in the two lines Hei $ D_{3} $ andHα quasi-simultaneously. The linear polarization of the lines is due to scattering of the anisotropic photospheric radiation, modified by the Hanle effect due to the local magnetic field. The interpretation of the polarization data in the two lines is able to provide the 3 components of the magnetic field vector, and one extra parameter, namely the electron density, because the linear polarization of Hα is also sensitive to the depolarizing effect of collisions with the electrons and protons of the medium. Moreover, by using two lines with different optical thicknesses, namely Hei $ D_{3} $, which is optically thin, and Hα, which is optically thick (τ = 1), it is possible to solve the fundamental ambiguity, each line providing two field vector solutions that are symmetrical in direction with respect to the line of sight in the case of the optically thin line, and which have a different symmetry in the case of the optically thick line. It is then possible to determine without ambiguity the polarity of the prominence magnetic field with respect to that of the photospheric field: 12 prominences are found to be Inverse polarity prominences, whereas 2 prominences are found to be Normal polarity prominences. It must be noticed that in 12 of the 14 cases, the line-of-sight component of the magnetic field vector has a Normal polarity (to the extent that the notion of polarity of a vector component is meaningful; no polarity can be derived in the 2 remaining cases); this may explain the controversy between the results obtained with methods based on the Hanle effect with results obtained through the Zeeman effect. A dip of the magnetic field lines across the prominence has been assumed, to which the optically thick Hα line is sensitive, and the optically thin Hei $ D_{3} $ line is insensitive. For the Inverse prominences, the average field strength is 7.5±1.2 G, the average angle,α, between the field vector and the prominence long axis is 36° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 29° ± 20°, and the average electron density is 2.1 × $ 10^{10} $ ± 0.7 × $ 10^{10} $ $ cm^{−3} $. For the Normal prominences, the average field strength is 13.2±2.0 G, the average angle,α, between the field vector and the prominence long axis is 53° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 0° ± 20° (horizontal field), and the average electron density is 8.7 × $ 10^{9} $ ± 3.0 × $ 10^{9} $ $ cm^{−3} $.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Field Vector</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Linear Polarization</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Polarization Data</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Solar Surface</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Normal Polarity</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Degl'Innocenti, Egidio Landi</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Leroy, Jean-Louis</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Sahal-Bréchot, Sylvie</subfield><subfield code="4">aut</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="t">Solar physics</subfield><subfield code="d">Kluwer Academic Publishers, 1967</subfield><subfield code="g">154(1994), 2 vom: Okt., Seite 231-260</subfield><subfield code="w">(DE-627)129856010</subfield><subfield code="w">(DE-600)281593-X</subfield><subfield code="w">(DE-576)015160033</subfield><subfield code="x">0038-0938</subfield><subfield code="7">nnns</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:154</subfield><subfield code="g">year:1994</subfield><subfield code="g">number:2</subfield><subfield code="g">month:10</subfield><subfield code="g">pages:231-260</subfield></datafield><datafield tag="856" ind1="4" ind2="1"><subfield code="u">https://doi.org/10.1007/BF00681098</subfield><subfield code="z">lizenzpflichtig</subfield><subfield code="3">Volltext</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_USEFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SYSFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_OLC</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-PHY</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-AST</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OPC-AST</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_11</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_22</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_40</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_47</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_70</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2002</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2279</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2286</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4012</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4306</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">154</subfield><subfield code="j">1994</subfield><subfield code="e">2</subfield><subfield code="c">10</subfield><subfield code="h">231-260</subfield></datafield></record></collection>
|
| author |
Bommier, Véronique |
| spellingShingle |
Bommier, Véronique ddc 530 ssgn 16,12 misc Field Vector misc Linear Polarization misc Polarization Data misc Solar Surface misc Normal Polarity Complete determination of the magnetic field vector and of the electron density in 14 prominences from linear polarizaton measurements in the HeI $ D_{3} $ and Hα lines |
| authorStr |
Bommier, Véronique |
| ppnlink_with_tag_str_mv |
@@773@@(DE-627)129856010 |
| format |
Article |
| dewey-ones |
530 - Physics |
| delete_txt_mv |
keep |
| author_role |
aut aut aut aut |
| collection |
OLC |
| remote_str |
false |
| illustrated |
Not Illustrated |
| issn |
0038-0938 |
| topic_title |
530 VZ 16,12 ssgn Complete determination of the magnetic field vector and of the electron density in 14 prominences from linear polarizaton measurements in the HeI $ D_{3} $ and Hα lines Field Vector Linear Polarization Polarization Data Solar Surface Normal Polarity |
| topic |
ddc 530 ssgn 16,12 misc Field Vector misc Linear Polarization misc Polarization Data misc Solar Surface misc Normal Polarity |
| topic_unstemmed |
ddc 530 ssgn 16,12 misc Field Vector misc Linear Polarization misc Polarization Data misc Solar Surface misc Normal Polarity |
| topic_browse |
ddc 530 ssgn 16,12 misc Field Vector misc Linear Polarization misc Polarization Data misc Solar Surface misc Normal Polarity |
| format_facet |
Aufsätze Gedruckte Aufsätze |
| format_main_str_mv |
Text Zeitschrift/Artikel |
| carriertype_str_mv |
nc |
| hierarchy_parent_title |
Solar physics |
| hierarchy_parent_id |
129856010 |
| dewey-tens |
530 - Physics |
| hierarchy_top_title |
Solar physics |
| isfreeaccess_txt |
false |
| familylinks_str_mv |
(DE-627)129856010 (DE-600)281593-X (DE-576)015160033 |
| title |
Complete determination of the magnetic field vector and of the electron density in 14 prominences from linear polarizaton measurements in the HeI $ D_{3} $ and Hα lines |
| ctrlnum |
(DE-627)OLC2033576558 (DE-He213)BF00681098-p |
| title_full |
Complete determination of the magnetic field vector and of the electron density in 14 prominences from linear polarizaton measurements in the HeI $ D_{3} $ and Hα lines |
| author_sort |
Bommier, Véronique |
| journal |
Solar physics |
| journalStr |
Solar physics |
| lang_code |
eng |
| isOA_bool |
false |
| dewey-hundreds |
500 - Science |
| recordtype |
marc |
| publishDateSort |
1994 |
| contenttype_str_mv |
txt |
| container_start_page |
231 |
| author_browse |
Bommier, Véronique Degl'Innocenti, Egidio Landi Leroy, Jean-Louis Sahal-Bréchot, Sylvie |
| container_volume |
154 |
| class |
530 VZ 16,12 ssgn |
| format_se |
Aufsätze |
| author-letter |
Bommier, Véronique |
| doi_str_mv |
10.1007/BF00681098 |
| dewey-full |
530 |
| title_sort |
complete determination of the magnetic field vector and of the electron density in 14 prominences from linear polarizaton measurements in the hei $ d_{3} $ and hα lines |
| title_auth |
Complete determination of the magnetic field vector and of the electron density in 14 prominences from linear polarizaton measurements in the HeI $ D_{3} $ and Hα lines |
| abstract |
Abstract The present paper is devoted to the interpretation of linear polarization data obtained in 14 quiescent prominences with the Pic-du-Midi coronagraph-polarimeter by J. L. Leroy, in the two lines Hei $ D_{3} $ andHα quasi-simultaneously. The linear polarization of the lines is due to scattering of the anisotropic photospheric radiation, modified by the Hanle effect due to the local magnetic field. The interpretation of the polarization data in the two lines is able to provide the 3 components of the magnetic field vector, and one extra parameter, namely the electron density, because the linear polarization of Hα is also sensitive to the depolarizing effect of collisions with the electrons and protons of the medium. Moreover, by using two lines with different optical thicknesses, namely Hei $ D_{3} $, which is optically thin, and Hα, which is optically thick (τ = 1), it is possible to solve the fundamental ambiguity, each line providing two field vector solutions that are symmetrical in direction with respect to the line of sight in the case of the optically thin line, and which have a different symmetry in the case of the optically thick line. It is then possible to determine without ambiguity the polarity of the prominence magnetic field with respect to that of the photospheric field: 12 prominences are found to be Inverse polarity prominences, whereas 2 prominences are found to be Normal polarity prominences. It must be noticed that in 12 of the 14 cases, the line-of-sight component of the magnetic field vector has a Normal polarity (to the extent that the notion of polarity of a vector component is meaningful; no polarity can be derived in the 2 remaining cases); this may explain the controversy between the results obtained with methods based on the Hanle effect with results obtained through the Zeeman effect. A dip of the magnetic field lines across the prominence has been assumed, to which the optically thick Hα line is sensitive, and the optically thin Hei $ D_{3} $ line is insensitive. For the Inverse prominences, the average field strength is 7.5±1.2 G, the average angle,α, between the field vector and the prominence long axis is 36° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 29° ± 20°, and the average electron density is 2.1 × $ 10^{10} $ ± 0.7 × $ 10^{10} $ $ cm^{−3} $. For the Normal prominences, the average field strength is 13.2±2.0 G, the average angle,α, between the field vector and the prominence long axis is 53° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 0° ± 20° (horizontal field), and the average electron density is 8.7 × $ 10^{9} $ ± 3.0 × $ 10^{9} $ $ cm^{−3} $. © Kluwer Academic Publishers 1994 |
| abstractGer |
Abstract The present paper is devoted to the interpretation of linear polarization data obtained in 14 quiescent prominences with the Pic-du-Midi coronagraph-polarimeter by J. L. Leroy, in the two lines Hei $ D_{3} $ andHα quasi-simultaneously. The linear polarization of the lines is due to scattering of the anisotropic photospheric radiation, modified by the Hanle effect due to the local magnetic field. The interpretation of the polarization data in the two lines is able to provide the 3 components of the magnetic field vector, and one extra parameter, namely the electron density, because the linear polarization of Hα is also sensitive to the depolarizing effect of collisions with the electrons and protons of the medium. Moreover, by using two lines with different optical thicknesses, namely Hei $ D_{3} $, which is optically thin, and Hα, which is optically thick (τ = 1), it is possible to solve the fundamental ambiguity, each line providing two field vector solutions that are symmetrical in direction with respect to the line of sight in the case of the optically thin line, and which have a different symmetry in the case of the optically thick line. It is then possible to determine without ambiguity the polarity of the prominence magnetic field with respect to that of the photospheric field: 12 prominences are found to be Inverse polarity prominences, whereas 2 prominences are found to be Normal polarity prominences. It must be noticed that in 12 of the 14 cases, the line-of-sight component of the magnetic field vector has a Normal polarity (to the extent that the notion of polarity of a vector component is meaningful; no polarity can be derived in the 2 remaining cases); this may explain the controversy between the results obtained with methods based on the Hanle effect with results obtained through the Zeeman effect. A dip of the magnetic field lines across the prominence has been assumed, to which the optically thick Hα line is sensitive, and the optically thin Hei $ D_{3} $ line is insensitive. For the Inverse prominences, the average field strength is 7.5±1.2 G, the average angle,α, between the field vector and the prominence long axis is 36° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 29° ± 20°, and the average electron density is 2.1 × $ 10^{10} $ ± 0.7 × $ 10^{10} $ $ cm^{−3} $. For the Normal prominences, the average field strength is 13.2±2.0 G, the average angle,α, between the field vector and the prominence long axis is 53° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 0° ± 20° (horizontal field), and the average electron density is 8.7 × $ 10^{9} $ ± 3.0 × $ 10^{9} $ $ cm^{−3} $. © Kluwer Academic Publishers 1994 |
| abstract_unstemmed |
Abstract The present paper is devoted to the interpretation of linear polarization data obtained in 14 quiescent prominences with the Pic-du-Midi coronagraph-polarimeter by J. L. Leroy, in the two lines Hei $ D_{3} $ andHα quasi-simultaneously. The linear polarization of the lines is due to scattering of the anisotropic photospheric radiation, modified by the Hanle effect due to the local magnetic field. The interpretation of the polarization data in the two lines is able to provide the 3 components of the magnetic field vector, and one extra parameter, namely the electron density, because the linear polarization of Hα is also sensitive to the depolarizing effect of collisions with the electrons and protons of the medium. Moreover, by using two lines with different optical thicknesses, namely Hei $ D_{3} $, which is optically thin, and Hα, which is optically thick (τ = 1), it is possible to solve the fundamental ambiguity, each line providing two field vector solutions that are symmetrical in direction with respect to the line of sight in the case of the optically thin line, and which have a different symmetry in the case of the optically thick line. It is then possible to determine without ambiguity the polarity of the prominence magnetic field with respect to that of the photospheric field: 12 prominences are found to be Inverse polarity prominences, whereas 2 prominences are found to be Normal polarity prominences. It must be noticed that in 12 of the 14 cases, the line-of-sight component of the magnetic field vector has a Normal polarity (to the extent that the notion of polarity of a vector component is meaningful; no polarity can be derived in the 2 remaining cases); this may explain the controversy between the results obtained with methods based on the Hanle effect with results obtained through the Zeeman effect. A dip of the magnetic field lines across the prominence has been assumed, to which the optically thick Hα line is sensitive, and the optically thin Hei $ D_{3} $ line is insensitive. For the Inverse prominences, the average field strength is 7.5±1.2 G, the average angle,α, between the field vector and the prominence long axis is 36° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 29° ± 20°, and the average electron density is 2.1 × $ 10^{10} $ ± 0.7 × $ 10^{10} $ $ cm^{−3} $. For the Normal prominences, the average field strength is 13.2±2.0 G, the average angle,α, between the field vector and the prominence long axis is 53° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 0° ± 20° (horizontal field), and the average electron density is 8.7 × $ 10^{9} $ ± 3.0 × $ 10^{9} $ $ cm^{−3} $. © Kluwer Academic Publishers 1994 |
| collection_details |
GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_22 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4306 |
| container_issue |
2 |
| title_short |
Complete determination of the magnetic field vector and of the electron density in 14 prominences from linear polarizaton measurements in the HeI $ D_{3} $ and Hα lines |
| url |
https://doi.org/10.1007/BF00681098 |
| remote_bool |
false |
| author2 |
Degl'Innocenti, Egidio Landi Leroy, Jean-Louis Sahal-Bréchot, Sylvie |
| author2Str |
Degl'Innocenti, Egidio Landi Leroy, Jean-Louis Sahal-Bréchot, Sylvie |
| ppnlink |
129856010 |
| mediatype_str_mv |
n |
| isOA_txt |
false |
| hochschulschrift_bool |
false |
| doi_str |
10.1007/BF00681098 |
| up_date |
2024-07-03T17:32:18.539Z |
| _version_ |
1803580015681470464 |
| fullrecord_marcxml |
<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">OLC2033576558</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230504045555.0</controlfield><controlfield tag="007">tu</controlfield><controlfield tag="008">200819s1994 xx ||||| 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1007/BF00681098</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)OLC2033576558</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-He213)BF00681098-p</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">530</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">16,12</subfield><subfield code="2">ssgn</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Bommier, Véronique</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Complete determination of the magnetic field vector and of the electron density in 14 prominences from linear polarizaton measurements in the HeI $ D_{3} $ and Hα lines</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">1994</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">ohne Hilfsmittel zu benutzen</subfield><subfield code="b">n</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Band</subfield><subfield code="b">nc</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="500" ind1=" " ind2=" "><subfield code="a">© Kluwer Academic Publishers 1994</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract The present paper is devoted to the interpretation of linear polarization data obtained in 14 quiescent prominences with the Pic-du-Midi coronagraph-polarimeter by J. L. Leroy, in the two lines Hei $ D_{3} $ andHα quasi-simultaneously. The linear polarization of the lines is due to scattering of the anisotropic photospheric radiation, modified by the Hanle effect due to the local magnetic field. The interpretation of the polarization data in the two lines is able to provide the 3 components of the magnetic field vector, and one extra parameter, namely the electron density, because the linear polarization of Hα is also sensitive to the depolarizing effect of collisions with the electrons and protons of the medium. Moreover, by using two lines with different optical thicknesses, namely Hei $ D_{3} $, which is optically thin, and Hα, which is optically thick (τ = 1), it is possible to solve the fundamental ambiguity, each line providing two field vector solutions that are symmetrical in direction with respect to the line of sight in the case of the optically thin line, and which have a different symmetry in the case of the optically thick line. It is then possible to determine without ambiguity the polarity of the prominence magnetic field with respect to that of the photospheric field: 12 prominences are found to be Inverse polarity prominences, whereas 2 prominences are found to be Normal polarity prominences. It must be noticed that in 12 of the 14 cases, the line-of-sight component of the magnetic field vector has a Normal polarity (to the extent that the notion of polarity of a vector component is meaningful; no polarity can be derived in the 2 remaining cases); this may explain the controversy between the results obtained with methods based on the Hanle effect with results obtained through the Zeeman effect. A dip of the magnetic field lines across the prominence has been assumed, to which the optically thick Hα line is sensitive, and the optically thin Hei $ D_{3} $ line is insensitive. For the Inverse prominences, the average field strength is 7.5±1.2 G, the average angle,α, between the field vector and the prominence long axis is 36° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 29° ± 20°, and the average electron density is 2.1 × $ 10^{10} $ ± 0.7 × $ 10^{10} $ $ cm^{−3} $. For the Normal prominences, the average field strength is 13.2±2.0 G, the average angle,α, between the field vector and the prominence long axis is 53° ± 15°, the average angle, ζ, between the outgoing field lines and the solar surface at the prominence boundary is 0° ± 20° (horizontal field), and the average electron density is 8.7 × $ 10^{9} $ ± 3.0 × $ 10^{9} $ $ cm^{−3} $.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Field Vector</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Linear Polarization</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Polarization Data</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Solar Surface</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Normal Polarity</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Degl'Innocenti, Egidio Landi</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Leroy, Jean-Louis</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Sahal-Bréchot, Sylvie</subfield><subfield code="4">aut</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="t">Solar physics</subfield><subfield code="d">Kluwer Academic Publishers, 1967</subfield><subfield code="g">154(1994), 2 vom: Okt., Seite 231-260</subfield><subfield code="w">(DE-627)129856010</subfield><subfield code="w">(DE-600)281593-X</subfield><subfield code="w">(DE-576)015160033</subfield><subfield code="x">0038-0938</subfield><subfield code="7">nnns</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:154</subfield><subfield code="g">year:1994</subfield><subfield code="g">number:2</subfield><subfield code="g">month:10</subfield><subfield code="g">pages:231-260</subfield></datafield><datafield tag="856" ind1="4" ind2="1"><subfield code="u">https://doi.org/10.1007/BF00681098</subfield><subfield code="z">lizenzpflichtig</subfield><subfield code="3">Volltext</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_USEFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SYSFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_OLC</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-PHY</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-AST</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OPC-AST</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_11</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_22</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_40</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_47</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_70</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2002</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2279</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2286</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4012</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4306</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">154</subfield><subfield code="j">1994</subfield><subfield code="e">2</subfield><subfield code="c">10</subfield><subfield code="h">231-260</subfield></datafield></record></collection>
|
| score |
7.400646 |