On the possibility of determining the coronal magnetic field from solar type III radio burst observations
Abstract A simple method of estimating the coronal magnetic field is suggested. It is based on the observational fact that the duration of the highly polarized part in type III bursts can be different, varying from a small fraction of the burst length to its total duration. We suggest that this diff...
Ausführliche Beschreibung
Gespeichert in:
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
1999 |
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| Umfang: |
12 |
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| Reproduktion: |
Springer Online Journal Archives 1860-2002 |
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| Übergeordnetes Werk: |
in: Solar physics - 1967, 185(1999) vom: Jan., Seite 193-204 |
| Übergeordnetes Werk: |
volume:185 ; year:1999 ; month:01 ; pages:193-204 ; extent:12 |
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NLEJ195867327 |
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| 245 | 1 | 0 | |a On the possibility of determining the coronal magnetic field from solar type III radio burst observations |
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| 520 | |a Abstract A simple method of estimating the coronal magnetic field is suggested. It is based on the observational fact that the duration of the highly polarized part in type III bursts can be different, varying from a small fraction of the burst length to its total duration. We suggest that this difference is determined by the relation between the size of the region where only the ordinary wave can propagate and the size of the region where the burst is generated at a fixed frequency. The magnetic field is estimated at several tens of gauss in regions emitting highly polarized type III bursts at frequencies over 200 MHz. Density and magnetic field scales are estimated. | ||
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| 700 | 1 | |a Ledenev, V.G. |4 oth | |
| 700 | 1 | |a Messerotti, M. |4 oth | |
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(DE-627)NLEJ195867327 DE-627 ger DE-627 rakwb eng On the possibility of determining the coronal magnetic field from solar type III radio burst observations 1999 12 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Abstract A simple method of estimating the coronal magnetic field is suggested. It is based on the observational fact that the duration of the highly polarized part in type III bursts can be different, varying from a small fraction of the burst length to its total duration. We suggest that this difference is determined by the relation between the size of the region where only the ordinary wave can propagate and the size of the region where the burst is generated at a fixed frequency. The magnetic field is estimated at several tens of gauss in regions emitting highly polarized type III bursts at frequencies over 200 MHz. Density and magnetic field scales are estimated. Springer Online Journal Archives 1860-2002 Ledenev, V.G. oth Messerotti, M. oth in Solar physics 1967 185(1999) vom: Jan., Seite 193-204 (DE-627)NLEJ188983465 (DE-600)1473830-2 1573-093X nnns volume:185 year:1999 month:01 pages:193-204 extent:12 http://dx.doi.org/10.1023/A:1005153005830 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 185 1999 1 193-204 12 |
| spelling |
(DE-627)NLEJ195867327 DE-627 ger DE-627 rakwb eng On the possibility of determining the coronal magnetic field from solar type III radio burst observations 1999 12 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Abstract A simple method of estimating the coronal magnetic field is suggested. It is based on the observational fact that the duration of the highly polarized part in type III bursts can be different, varying from a small fraction of the burst length to its total duration. We suggest that this difference is determined by the relation between the size of the region where only the ordinary wave can propagate and the size of the region where the burst is generated at a fixed frequency. The magnetic field is estimated at several tens of gauss in regions emitting highly polarized type III bursts at frequencies over 200 MHz. Density and magnetic field scales are estimated. Springer Online Journal Archives 1860-2002 Ledenev, V.G. oth Messerotti, M. oth in Solar physics 1967 185(1999) vom: Jan., Seite 193-204 (DE-627)NLEJ188983465 (DE-600)1473830-2 1573-093X nnns volume:185 year:1999 month:01 pages:193-204 extent:12 http://dx.doi.org/10.1023/A:1005153005830 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 185 1999 1 193-204 12 |
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(DE-627)NLEJ195867327 DE-627 ger DE-627 rakwb eng On the possibility of determining the coronal magnetic field from solar type III radio burst observations 1999 12 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Abstract A simple method of estimating the coronal magnetic field is suggested. It is based on the observational fact that the duration of the highly polarized part in type III bursts can be different, varying from a small fraction of the burst length to its total duration. We suggest that this difference is determined by the relation between the size of the region where only the ordinary wave can propagate and the size of the region where the burst is generated at a fixed frequency. The magnetic field is estimated at several tens of gauss in regions emitting highly polarized type III bursts at frequencies over 200 MHz. Density and magnetic field scales are estimated. Springer Online Journal Archives 1860-2002 Ledenev, V.G. oth Messerotti, M. oth in Solar physics 1967 185(1999) vom: Jan., Seite 193-204 (DE-627)NLEJ188983465 (DE-600)1473830-2 1573-093X nnns volume:185 year:1999 month:01 pages:193-204 extent:12 http://dx.doi.org/10.1023/A:1005153005830 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 185 1999 1 193-204 12 |
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(DE-627)NLEJ195867327 DE-627 ger DE-627 rakwb eng On the possibility of determining the coronal magnetic field from solar type III radio burst observations 1999 12 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Abstract A simple method of estimating the coronal magnetic field is suggested. It is based on the observational fact that the duration of the highly polarized part in type III bursts can be different, varying from a small fraction of the burst length to its total duration. We suggest that this difference is determined by the relation between the size of the region where only the ordinary wave can propagate and the size of the region where the burst is generated at a fixed frequency. The magnetic field is estimated at several tens of gauss in regions emitting highly polarized type III bursts at frequencies over 200 MHz. Density and magnetic field scales are estimated. Springer Online Journal Archives 1860-2002 Ledenev, V.G. oth Messerotti, M. oth in Solar physics 1967 185(1999) vom: Jan., Seite 193-204 (DE-627)NLEJ188983465 (DE-600)1473830-2 1573-093X nnns volume:185 year:1999 month:01 pages:193-204 extent:12 http://dx.doi.org/10.1023/A:1005153005830 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 185 1999 1 193-204 12 |
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(DE-627)NLEJ195867327 DE-627 ger DE-627 rakwb eng On the possibility of determining the coronal magnetic field from solar type III radio burst observations 1999 12 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier Abstract A simple method of estimating the coronal magnetic field is suggested. It is based on the observational fact that the duration of the highly polarized part in type III bursts can be different, varying from a small fraction of the burst length to its total duration. We suggest that this difference is determined by the relation between the size of the region where only the ordinary wave can propagate and the size of the region where the burst is generated at a fixed frequency. The magnetic field is estimated at several tens of gauss in regions emitting highly polarized type III bursts at frequencies over 200 MHz. Density and magnetic field scales are estimated. Springer Online Journal Archives 1860-2002 Ledenev, V.G. oth Messerotti, M. oth in Solar physics 1967 185(1999) vom: Jan., Seite 193-204 (DE-627)NLEJ188983465 (DE-600)1473830-2 1573-093X nnns volume:185 year:1999 month:01 pages:193-204 extent:12 http://dx.doi.org/10.1023/A:1005153005830 GBV_USEFLAG_U ZDB-1-SOJ GBV_NL_ARTICLE AR 185 1999 1 193-204 12 |
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On the possibility of determining the coronal magnetic field from solar type III radio burst observations |
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Abstract A simple method of estimating the coronal magnetic field is suggested. It is based on the observational fact that the duration of the highly polarized part in type III bursts can be different, varying from a small fraction of the burst length to its total duration. We suggest that this difference is determined by the relation between the size of the region where only the ordinary wave can propagate and the size of the region where the burst is generated at a fixed frequency. The magnetic field is estimated at several tens of gauss in regions emitting highly polarized type III bursts at frequencies over 200 MHz. Density and magnetic field scales are estimated. |
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Abstract A simple method of estimating the coronal magnetic field is suggested. It is based on the observational fact that the duration of the highly polarized part in type III bursts can be different, varying from a small fraction of the burst length to its total duration. We suggest that this difference is determined by the relation between the size of the region where only the ordinary wave can propagate and the size of the region where the burst is generated at a fixed frequency. The magnetic field is estimated at several tens of gauss in regions emitting highly polarized type III bursts at frequencies over 200 MHz. Density and magnetic field scales are estimated. |
| abstract_unstemmed |
Abstract A simple method of estimating the coronal magnetic field is suggested. It is based on the observational fact that the duration of the highly polarized part in type III bursts can be different, varying from a small fraction of the burst length to its total duration. We suggest that this difference is determined by the relation between the size of the region where only the ordinary wave can propagate and the size of the region where the burst is generated at a fixed frequency. The magnetic field is estimated at several tens of gauss in regions emitting highly polarized type III bursts at frequencies over 200 MHz. Density and magnetic field scales are estimated. |
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On the possibility of determining the coronal magnetic field from solar type III radio burst observations |
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