Polarization changes with time during solar microwave impulsive bursts

Abstract The evolution with time of circular polarization π(t) from solar bursts at 7 GHz presents, in the majority of cases, a polarization degree peak before the maximum flux time. The subsequent evolution of π(t) is continuous and usually increasing. The changes could be caused by superimposed po...
Ausführliche Beschreibung

Gespeichert in:

Autor*in:	Kaufmann, Pierre [verfasserIn] Matsuura, Oscar T. Dos Santos, P. Marques

Format:	Artikel
Sprache:	Englisch

Erschienen:	1970

Schlagwörter:	Microwave Flare Propagation Effect Subsequent Evolution Polarization Effect

Anmerkung:	© D. Reidel Publishing Company 1970

Übergeordnetes Werk:	Enthalten in: Solar physics - Kluwer Academic Publishers, 1967, 14(1970), 1 vom: Sept., Seite 190-195
Übergeordnetes Werk:	volume:14 ; year:1970 ; number:1 ; month:09 ; pages:190-195

Links:	Volltext

DOI / URN:	10.1007/BF00240177

Katalog-ID:	OLC2033522687

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520			\|a Abstract The evolution with time of circular polarization π(t) from solar bursts at 7 GHz presents, in the majority of cases, a polarization degree peak before the maximum flux time. The subsequent evolution of π(t) is continuous and usually increasing. The changes could be caused by superimposed polarization effects, due to the fast emissive electrons (dominant in the first phase), and to the propagation effects caused by the coronal condensation where the event occurred (dominant in the second phase). In an approximate approach, π(t) is connected to the movement of the source in the second phase, being qualitatively sound, but limited to the lack of knowledge on acceleration processes and on magnetic field topology in the active region where the flares take place.
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allfields	10.1007/BF00240177 doi (DE-627)OLC2033522687 (DE-He213)BF00240177-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Kaufmann, Pierre verfasserin aut Polarization changes with time during solar microwave impulsive bursts 1970 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1970 Abstract The evolution with time of circular polarization π(t) from solar bursts at 7 GHz presents, in the majority of cases, a polarization degree peak before the maximum flux time. The subsequent evolution of π(t) is continuous and usually increasing. The changes could be caused by superimposed polarization effects, due to the fast emissive electrons (dominant in the first phase), and to the propagation effects caused by the coronal condensation where the event occurred (dominant in the second phase). In an approximate approach, π(t) is connected to the movement of the source in the second phase, being qualitatively sound, but limited to the lack of knowledge on acceleration processes and on magnetic field topology in the active region where the flares take place. Microwave Flare Propagation Effect Subsequent Evolution Polarization Effect Matsuura, Oscar T. aut Dos Santos, P. Marques aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 14(1970), 1 vom: Sept., Seite 190-195 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:14 year:1970 number:1 month:09 pages:190-195 https://doi.org/10.1007/BF00240177 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_170 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4306 AR 14 1970 1 09 190-195
spelling	10.1007/BF00240177 doi (DE-627)OLC2033522687 (DE-He213)BF00240177-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Kaufmann, Pierre verfasserin aut Polarization changes with time during solar microwave impulsive bursts 1970 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1970 Abstract The evolution with time of circular polarization π(t) from solar bursts at 7 GHz presents, in the majority of cases, a polarization degree peak before the maximum flux time. The subsequent evolution of π(t) is continuous and usually increasing. The changes could be caused by superimposed polarization effects, due to the fast emissive electrons (dominant in the first phase), and to the propagation effects caused by the coronal condensation where the event occurred (dominant in the second phase). In an approximate approach, π(t) is connected to the movement of the source in the second phase, being qualitatively sound, but limited to the lack of knowledge on acceleration processes and on magnetic field topology in the active region where the flares take place. Microwave Flare Propagation Effect Subsequent Evolution Polarization Effect Matsuura, Oscar T. aut Dos Santos, P. Marques aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 14(1970), 1 vom: Sept., Seite 190-195 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:14 year:1970 number:1 month:09 pages:190-195 https://doi.org/10.1007/BF00240177 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_170 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4306 AR 14 1970 1 09 190-195
allfields_unstemmed	10.1007/BF00240177 doi (DE-627)OLC2033522687 (DE-He213)BF00240177-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Kaufmann, Pierre verfasserin aut Polarization changes with time during solar microwave impulsive bursts 1970 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1970 Abstract The evolution with time of circular polarization π(t) from solar bursts at 7 GHz presents, in the majority of cases, a polarization degree peak before the maximum flux time. The subsequent evolution of π(t) is continuous and usually increasing. The changes could be caused by superimposed polarization effects, due to the fast emissive electrons (dominant in the first phase), and to the propagation effects caused by the coronal condensation where the event occurred (dominant in the second phase). In an approximate approach, π(t) is connected to the movement of the source in the second phase, being qualitatively sound, but limited to the lack of knowledge on acceleration processes and on magnetic field topology in the active region where the flares take place. Microwave Flare Propagation Effect Subsequent Evolution Polarization Effect Matsuura, Oscar T. aut Dos Santos, P. Marques aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 14(1970), 1 vom: Sept., Seite 190-195 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:14 year:1970 number:1 month:09 pages:190-195 https://doi.org/10.1007/BF00240177 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_170 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4306 AR 14 1970 1 09 190-195
allfieldsGer	10.1007/BF00240177 doi (DE-627)OLC2033522687 (DE-He213)BF00240177-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Kaufmann, Pierre verfasserin aut Polarization changes with time during solar microwave impulsive bursts 1970 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1970 Abstract The evolution with time of circular polarization π(t) from solar bursts at 7 GHz presents, in the majority of cases, a polarization degree peak before the maximum flux time. The subsequent evolution of π(t) is continuous and usually increasing. The changes could be caused by superimposed polarization effects, due to the fast emissive electrons (dominant in the first phase), and to the propagation effects caused by the coronal condensation where the event occurred (dominant in the second phase). In an approximate approach, π(t) is connected to the movement of the source in the second phase, being qualitatively sound, but limited to the lack of knowledge on acceleration processes and on magnetic field topology in the active region where the flares take place. Microwave Flare Propagation Effect Subsequent Evolution Polarization Effect Matsuura, Oscar T. aut Dos Santos, P. Marques aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 14(1970), 1 vom: Sept., Seite 190-195 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:14 year:1970 number:1 month:09 pages:190-195 https://doi.org/10.1007/BF00240177 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_170 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4306 AR 14 1970 1 09 190-195
allfieldsSound	10.1007/BF00240177 doi (DE-627)OLC2033522687 (DE-He213)BF00240177-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Kaufmann, Pierre verfasserin aut Polarization changes with time during solar microwave impulsive bursts 1970 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Company 1970 Abstract The evolution with time of circular polarization π(t) from solar bursts at 7 GHz presents, in the majority of cases, a polarization degree peak before the maximum flux time. The subsequent evolution of π(t) is continuous and usually increasing. The changes could be caused by superimposed polarization effects, due to the fast emissive electrons (dominant in the first phase), and to the propagation effects caused by the coronal condensation where the event occurred (dominant in the second phase). In an approximate approach, π(t) is connected to the movement of the source in the second phase, being qualitatively sound, but limited to the lack of knowledge on acceleration processes and on magnetic field topology in the active region where the flares take place. Microwave Flare Propagation Effect Subsequent Evolution Polarization Effect Matsuura, Oscar T. aut Dos Santos, P. Marques aut Enthalten in Solar physics Kluwer Academic Publishers, 1967 14(1970), 1 vom: Sept., Seite 190-195 (DE-627)129856010 (DE-600)281593-X (DE-576)015160033 0038-0938 nnns volume:14 year:1970 number:1 month:09 pages:190-195 https://doi.org/10.1007/BF00240177 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_170 GBV_ILN_2002 GBV_ILN_2006 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4306 AR 14 1970 1 09 190-195
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title	Polarization changes with time during solar microwave impulsive bursts
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title_sort	polarization changes with time during solar microwave impulsive bursts
title_auth	Polarization changes with time during solar microwave impulsive bursts
abstract	Abstract The evolution with time of circular polarization π(t) from solar bursts at 7 GHz presents, in the majority of cases, a polarization degree peak before the maximum flux time. The subsequent evolution of π(t) is continuous and usually increasing. The changes could be caused by superimposed polarization effects, due to the fast emissive electrons (dominant in the first phase), and to the propagation effects caused by the coronal condensation where the event occurred (dominant in the second phase). In an approximate approach, π(t) is connected to the movement of the source in the second phase, being qualitatively sound, but limited to the lack of knowledge on acceleration processes and on magnetic field topology in the active region where the flares take place. © D. Reidel Publishing Company 1970
abstractGer	Abstract The evolution with time of circular polarization π(t) from solar bursts at 7 GHz presents, in the majority of cases, a polarization degree peak before the maximum flux time. The subsequent evolution of π(t) is continuous and usually increasing. The changes could be caused by superimposed polarization effects, due to the fast emissive electrons (dominant in the first phase), and to the propagation effects caused by the coronal condensation where the event occurred (dominant in the second phase). In an approximate approach, π(t) is connected to the movement of the source in the second phase, being qualitatively sound, but limited to the lack of knowledge on acceleration processes and on magnetic field topology in the active region where the flares take place. © D. Reidel Publishing Company 1970
abstract_unstemmed	Abstract The evolution with time of circular polarization π(t) from solar bursts at 7 GHz presents, in the majority of cases, a polarization degree peak before the maximum flux time. The subsequent evolution of π(t) is continuous and usually increasing. The changes could be caused by superimposed polarization effects, due to the fast emissive electrons (dominant in the first phase), and to the propagation effects caused by the coronal condensation where the event occurred (dominant in the second phase). In an approximate approach, π(t) is connected to the movement of the source in the second phase, being qualitatively sound, but limited to the lack of knowledge on acceleration processes and on magnetic field topology in the active region where the flares take place. © D. Reidel Publishing Company 1970
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container_issue	1
title_short	Polarization changes with time during solar microwave impulsive bursts
url	https://doi.org/10.1007/BF00240177
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author2	Matsuura, Oscar T. Dos Santos, P. Marques
author2Str	Matsuura, Oscar T. Dos Santos, P. Marques
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up_date	2024-07-03T17:19:08.522Z
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