Dynamic variations of the outer radiation belt during magnetic storms for 1.5–6.0 MeV electrons

Abstract The CME’s structure of solar wind (interplanetary magnetic field) is different from CIR’s. The two processes in which plasma and solar wind energy are injected into the Earth’s inner magnetosphere are not the same. So, the variations of energetic electrons flux in the radiation belts are di...
Ausführliche Beschreibung

Gespeichert in:

Autor*in:	Yuan, ChongJing [verfasserIn] Zong, QiuGang [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2011

Schlagwörter:	outer radiation belt relativistic electrons magnetic storms CME CIR energetic particles

Übergeordnetes Werk:	Enthalten in: Science in China - Heidelberg : Springer, 1997, 54(2011), 2 vom: Feb., Seite 431-440
Übergeordnetes Werk:	volume:54 ; year:2011 ; number:2 ; month:02 ; pages:431-440

Links:	Volltext

DOI / URN:	10.1007/s11431-010-4269-9

Katalog-ID:	SPR019269595

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520			\|a Abstract The CME’s structure of solar wind (interplanetary magnetic field) is different from CIR’s. The two processes in which plasma and solar wind energy are injected into the Earth’s inner magnetosphere are not the same. So, the variations of energetic electrons flux in the radiation belts are different between the storms associated with CMEs and CIRs. By using data from SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer) satellite, we have investigated the dynamic variations of the outer radiation belt for 1.5–6.0 MeV electrons during 54 CME-driven storms and 26 CIR-driven recurrent storms. According to the superposed epoch analysis, for CME- and CIR-driven storms, when the Dst index reaches the minimum, the locations of the outer boundary move to L=4 and L=5.5, respectively. In the recovery phases, the locations of the outer boundary of the outer radiation belt are generally lower than and slightly higher than those before CME- and CIR-driven storms, respectively. We have found that the logarithmically decaying 1/e cut-off L-shell is a satisfying indicator of the outer boundary of the outer radiation belt. Furthermore, our study shows that the logarithmically decaying 1/e cut-off latitude is dependent on the Kp index in the main phases of CME- and CIR- driven storms, while in the recovery phases, there is no obvious correlation. In addition, it has been shown that the locations of the peak electron flux are controlled by the minimum Dst index in the main phases of CME-driven storms. The influences of multiple storms on the electron flux of outer radiation belt have also been investigated.
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matchkey_str	article:1862281X:2011----::yaivrainoteuerdainetuigantct
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allfields	10.1007/s11431-010-4269-9 doi (DE-627)SPR019269595 (SPR)s11431-010-4269-9-e DE-627 ger DE-627 rakwb eng 600 ASE 600 ASE 50.00 bkl Yuan, ChongJing verfasserin aut Dynamic variations of the outer radiation belt during magnetic storms for 1.5–6.0 MeV electrons 2011 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The CME’s structure of solar wind (interplanetary magnetic field) is different from CIR’s. The two processes in which plasma and solar wind energy are injected into the Earth’s inner magnetosphere are not the same. So, the variations of energetic electrons flux in the radiation belts are different between the storms associated with CMEs and CIRs. By using data from SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer) satellite, we have investigated the dynamic variations of the outer radiation belt for 1.5–6.0 MeV electrons during 54 CME-driven storms and 26 CIR-driven recurrent storms. According to the superposed epoch analysis, for CME- and CIR-driven storms, when the Dst index reaches the minimum, the locations of the outer boundary move to L=4 and L=5.5, respectively. In the recovery phases, the locations of the outer boundary of the outer radiation belt are generally lower than and slightly higher than those before CME- and CIR-driven storms, respectively. We have found that the logarithmically decaying 1/e cut-off L-shell is a satisfying indicator of the outer boundary of the outer radiation belt. Furthermore, our study shows that the logarithmically decaying 1/e cut-off latitude is dependent on the Kp index in the main phases of CME- and CIR- driven storms, while in the recovery phases, there is no obvious correlation. In addition, it has been shown that the locations of the peak electron flux are controlled by the minimum Dst index in the main phases of CME-driven storms. The influences of multiple storms on the electron flux of outer radiation belt have also been investigated. outer radiation belt (dpeaa)DE-He213 relativistic electrons (dpeaa)DE-He213 magnetic storms (dpeaa)DE-He213 CME (dpeaa)DE-He213 CIR (dpeaa)DE-He213 energetic particles (dpeaa)DE-He213 Zong, QiuGang verfasserin aut Enthalten in Science in China Heidelberg : Springer, 1997 54(2011), 2 vom: Feb., Seite 431-440 (DE-627)385614756 (DE-600)2142897-9 1862-281X nnns volume:54 year:2011 number:2 month:02 pages:431-440 https://dx.doi.org/10.1007/s11431-010-4269-9 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_152 GBV_ILN_161 GBV_ILN_171 GBV_ILN_187 GBV_ILN_224 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 50.00 ASE AR 54 2011 2 02 431-440
spelling	10.1007/s11431-010-4269-9 doi (DE-627)SPR019269595 (SPR)s11431-010-4269-9-e DE-627 ger DE-627 rakwb eng 600 ASE 600 ASE 50.00 bkl Yuan, ChongJing verfasserin aut Dynamic variations of the outer radiation belt during magnetic storms for 1.5–6.0 MeV electrons 2011 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The CME’s structure of solar wind (interplanetary magnetic field) is different from CIR’s. The two processes in which plasma and solar wind energy are injected into the Earth’s inner magnetosphere are not the same. So, the variations of energetic electrons flux in the radiation belts are different between the storms associated with CMEs and CIRs. By using data from SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer) satellite, we have investigated the dynamic variations of the outer radiation belt for 1.5–6.0 MeV electrons during 54 CME-driven storms and 26 CIR-driven recurrent storms. According to the superposed epoch analysis, for CME- and CIR-driven storms, when the Dst index reaches the minimum, the locations of the outer boundary move to L=4 and L=5.5, respectively. In the recovery phases, the locations of the outer boundary of the outer radiation belt are generally lower than and slightly higher than those before CME- and CIR-driven storms, respectively. We have found that the logarithmically decaying 1/e cut-off L-shell is a satisfying indicator of the outer boundary of the outer radiation belt. Furthermore, our study shows that the logarithmically decaying 1/e cut-off latitude is dependent on the Kp index in the main phases of CME- and CIR- driven storms, while in the recovery phases, there is no obvious correlation. In addition, it has been shown that the locations of the peak electron flux are controlled by the minimum Dst index in the main phases of CME-driven storms. The influences of multiple storms on the electron flux of outer radiation belt have also been investigated. outer radiation belt (dpeaa)DE-He213 relativistic electrons (dpeaa)DE-He213 magnetic storms (dpeaa)DE-He213 CME (dpeaa)DE-He213 CIR (dpeaa)DE-He213 energetic particles (dpeaa)DE-He213 Zong, QiuGang verfasserin aut Enthalten in Science in China Heidelberg : Springer, 1997 54(2011), 2 vom: Feb., Seite 431-440 (DE-627)385614756 (DE-600)2142897-9 1862-281X nnns volume:54 year:2011 number:2 month:02 pages:431-440 https://dx.doi.org/10.1007/s11431-010-4269-9 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_152 GBV_ILN_161 GBV_ILN_171 GBV_ILN_187 GBV_ILN_224 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 50.00 ASE AR 54 2011 2 02 431-440
allfields_unstemmed	10.1007/s11431-010-4269-9 doi (DE-627)SPR019269595 (SPR)s11431-010-4269-9-e DE-627 ger DE-627 rakwb eng 600 ASE 600 ASE 50.00 bkl Yuan, ChongJing verfasserin aut Dynamic variations of the outer radiation belt during magnetic storms for 1.5–6.0 MeV electrons 2011 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The CME’s structure of solar wind (interplanetary magnetic field) is different from CIR’s. The two processes in which plasma and solar wind energy are injected into the Earth’s inner magnetosphere are not the same. So, the variations of energetic electrons flux in the radiation belts are different between the storms associated with CMEs and CIRs. By using data from SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer) satellite, we have investigated the dynamic variations of the outer radiation belt for 1.5–6.0 MeV electrons during 54 CME-driven storms and 26 CIR-driven recurrent storms. According to the superposed epoch analysis, for CME- and CIR-driven storms, when the Dst index reaches the minimum, the locations of the outer boundary move to L=4 and L=5.5, respectively. In the recovery phases, the locations of the outer boundary of the outer radiation belt are generally lower than and slightly higher than those before CME- and CIR-driven storms, respectively. We have found that the logarithmically decaying 1/e cut-off L-shell is a satisfying indicator of the outer boundary of the outer radiation belt. Furthermore, our study shows that the logarithmically decaying 1/e cut-off latitude is dependent on the Kp index in the main phases of CME- and CIR- driven storms, while in the recovery phases, there is no obvious correlation. In addition, it has been shown that the locations of the peak electron flux are controlled by the minimum Dst index in the main phases of CME-driven storms. The influences of multiple storms on the electron flux of outer radiation belt have also been investigated. outer radiation belt (dpeaa)DE-He213 relativistic electrons (dpeaa)DE-He213 magnetic storms (dpeaa)DE-He213 CME (dpeaa)DE-He213 CIR (dpeaa)DE-He213 energetic particles (dpeaa)DE-He213 Zong, QiuGang verfasserin aut Enthalten in Science in China Heidelberg : Springer, 1997 54(2011), 2 vom: Feb., Seite 431-440 (DE-627)385614756 (DE-600)2142897-9 1862-281X nnns volume:54 year:2011 number:2 month:02 pages:431-440 https://dx.doi.org/10.1007/s11431-010-4269-9 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_152 GBV_ILN_161 GBV_ILN_171 GBV_ILN_187 GBV_ILN_224 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 50.00 ASE AR 54 2011 2 02 431-440
allfieldsGer	10.1007/s11431-010-4269-9 doi (DE-627)SPR019269595 (SPR)s11431-010-4269-9-e DE-627 ger DE-627 rakwb eng 600 ASE 600 ASE 50.00 bkl Yuan, ChongJing verfasserin aut Dynamic variations of the outer radiation belt during magnetic storms for 1.5–6.0 MeV electrons 2011 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The CME’s structure of solar wind (interplanetary magnetic field) is different from CIR’s. The two processes in which plasma and solar wind energy are injected into the Earth’s inner magnetosphere are not the same. So, the variations of energetic electrons flux in the radiation belts are different between the storms associated with CMEs and CIRs. By using data from SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer) satellite, we have investigated the dynamic variations of the outer radiation belt for 1.5–6.0 MeV electrons during 54 CME-driven storms and 26 CIR-driven recurrent storms. According to the superposed epoch analysis, for CME- and CIR-driven storms, when the Dst index reaches the minimum, the locations of the outer boundary move to L=4 and L=5.5, respectively. In the recovery phases, the locations of the outer boundary of the outer radiation belt are generally lower than and slightly higher than those before CME- and CIR-driven storms, respectively. We have found that the logarithmically decaying 1/e cut-off L-shell is a satisfying indicator of the outer boundary of the outer radiation belt. Furthermore, our study shows that the logarithmically decaying 1/e cut-off latitude is dependent on the Kp index in the main phases of CME- and CIR- driven storms, while in the recovery phases, there is no obvious correlation. In addition, it has been shown that the locations of the peak electron flux are controlled by the minimum Dst index in the main phases of CME-driven storms. The influences of multiple storms on the electron flux of outer radiation belt have also been investigated. outer radiation belt (dpeaa)DE-He213 relativistic electrons (dpeaa)DE-He213 magnetic storms (dpeaa)DE-He213 CME (dpeaa)DE-He213 CIR (dpeaa)DE-He213 energetic particles (dpeaa)DE-He213 Zong, QiuGang verfasserin aut Enthalten in Science in China Heidelberg : Springer, 1997 54(2011), 2 vom: Feb., Seite 431-440 (DE-627)385614756 (DE-600)2142897-9 1862-281X nnns volume:54 year:2011 number:2 month:02 pages:431-440 https://dx.doi.org/10.1007/s11431-010-4269-9 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_152 GBV_ILN_161 GBV_ILN_171 GBV_ILN_187 GBV_ILN_224 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 50.00 ASE AR 54 2011 2 02 431-440
allfieldsSound	10.1007/s11431-010-4269-9 doi (DE-627)SPR019269595 (SPR)s11431-010-4269-9-e DE-627 ger DE-627 rakwb eng 600 ASE 600 ASE 50.00 bkl Yuan, ChongJing verfasserin aut Dynamic variations of the outer radiation belt during magnetic storms for 1.5–6.0 MeV electrons 2011 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The CME’s structure of solar wind (interplanetary magnetic field) is different from CIR’s. The two processes in which plasma and solar wind energy are injected into the Earth’s inner magnetosphere are not the same. So, the variations of energetic electrons flux in the radiation belts are different between the storms associated with CMEs and CIRs. By using data from SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer) satellite, we have investigated the dynamic variations of the outer radiation belt for 1.5–6.0 MeV electrons during 54 CME-driven storms and 26 CIR-driven recurrent storms. According to the superposed epoch analysis, for CME- and CIR-driven storms, when the Dst index reaches the minimum, the locations of the outer boundary move to L=4 and L=5.5, respectively. In the recovery phases, the locations of the outer boundary of the outer radiation belt are generally lower than and slightly higher than those before CME- and CIR-driven storms, respectively. We have found that the logarithmically decaying 1/e cut-off L-shell is a satisfying indicator of the outer boundary of the outer radiation belt. Furthermore, our study shows that the logarithmically decaying 1/e cut-off latitude is dependent on the Kp index in the main phases of CME- and CIR- driven storms, while in the recovery phases, there is no obvious correlation. In addition, it has been shown that the locations of the peak electron flux are controlled by the minimum Dst index in the main phases of CME-driven storms. The influences of multiple storms on the electron flux of outer radiation belt have also been investigated. outer radiation belt (dpeaa)DE-He213 relativistic electrons (dpeaa)DE-He213 magnetic storms (dpeaa)DE-He213 CME (dpeaa)DE-He213 CIR (dpeaa)DE-He213 energetic particles (dpeaa)DE-He213 Zong, QiuGang verfasserin aut Enthalten in Science in China Heidelberg : Springer, 1997 54(2011), 2 vom: Feb., Seite 431-440 (DE-627)385614756 (DE-600)2142897-9 1862-281X nnns volume:54 year:2011 number:2 month:02 pages:431-440 https://dx.doi.org/10.1007/s11431-010-4269-9 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_152 GBV_ILN_161 GBV_ILN_171 GBV_ILN_187 GBV_ILN_224 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 50.00 ASE AR 54 2011 2 02 431-440
language	English
source	Enthalten in Science in China 54(2011), 2 vom: Feb., Seite 431-440 volume:54 year:2011 number:2 month:02 pages:431-440
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authorswithroles_txt_mv	Yuan, ChongJing @@aut@@ Zong, QiuGang @@aut@@
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The two processes in which plasma and solar wind energy are injected into the Earth’s inner magnetosphere are not the same. So, the variations of energetic electrons flux in the radiation belts are different between the storms associated with CMEs and CIRs. By using data from SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer) satellite, we have investigated the dynamic variations of the outer radiation belt for 1.5–6.0 MeV electrons during 54 CME-driven storms and 26 CIR-driven recurrent storms. According to the superposed epoch analysis, for CME- and CIR-driven storms, when the Dst index reaches the minimum, the locations of the outer boundary move to L=4 and L=5.5, respectively. In the recovery phases, the locations of the outer boundary of the outer radiation belt are generally lower than and slightly higher than those before CME- and CIR-driven storms, respectively. We have found that the logarithmically decaying 1/e cut-off L-shell is a satisfying indicator of the outer boundary of the outer radiation belt. Furthermore, our study shows that the logarithmically decaying 1/e cut-off latitude is dependent on the Kp index in the main phases of CME- and CIR- driven storms, while in the recovery phases, there is no obvious correlation. In addition, it has been shown that the locations of the peak electron flux are controlled by the minimum Dst index in the main phases of CME-driven storms. 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author	Yuan, ChongJing
spellingShingle	Yuan, ChongJing ddc 600 bkl 50.00 misc outer radiation belt misc relativistic electrons misc magnetic storms misc CME misc CIR misc energetic particles Dynamic variations of the outer radiation belt during magnetic storms for 1.5–6.0 MeV electrons
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topic_title	600 ASE 50.00 bkl Dynamic variations of the outer radiation belt during magnetic storms for 1.5–6.0 MeV electrons outer radiation belt (dpeaa)DE-He213 relativistic electrons (dpeaa)DE-He213 magnetic storms (dpeaa)DE-He213 CME (dpeaa)DE-He213 CIR (dpeaa)DE-He213 energetic particles (dpeaa)DE-He213
topic	ddc 600 bkl 50.00 misc outer radiation belt misc relativistic electrons misc magnetic storms misc CME misc CIR misc energetic particles
topic_unstemmed	ddc 600 bkl 50.00 misc outer radiation belt misc relativistic electrons misc magnetic storms misc CME misc CIR misc energetic particles
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title	Dynamic variations of the outer radiation belt during magnetic storms for 1.5–6.0 MeV electrons
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title_full	Dynamic variations of the outer radiation belt during magnetic storms for 1.5–6.0 MeV electrons
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title_sort	dynamic variations of the outer radiation belt during magnetic storms for 1.5–6.0 mev electrons
title_auth	Dynamic variations of the outer radiation belt during magnetic storms for 1.5–6.0 MeV electrons
abstract	Abstract The CME’s structure of solar wind (interplanetary magnetic field) is different from CIR’s. The two processes in which plasma and solar wind energy are injected into the Earth’s inner magnetosphere are not the same. So, the variations of energetic electrons flux in the radiation belts are different between the storms associated with CMEs and CIRs. By using data from SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer) satellite, we have investigated the dynamic variations of the outer radiation belt for 1.5–6.0 MeV electrons during 54 CME-driven storms and 26 CIR-driven recurrent storms. According to the superposed epoch analysis, for CME- and CIR-driven storms, when the Dst index reaches the minimum, the locations of the outer boundary move to L=4 and L=5.5, respectively. In the recovery phases, the locations of the outer boundary of the outer radiation belt are generally lower than and slightly higher than those before CME- and CIR-driven storms, respectively. We have found that the logarithmically decaying 1/e cut-off L-shell is a satisfying indicator of the outer boundary of the outer radiation belt. Furthermore, our study shows that the logarithmically decaying 1/e cut-off latitude is dependent on the Kp index in the main phases of CME- and CIR- driven storms, while in the recovery phases, there is no obvious correlation. In addition, it has been shown that the locations of the peak electron flux are controlled by the minimum Dst index in the main phases of CME-driven storms. The influences of multiple storms on the electron flux of outer radiation belt have also been investigated.
abstractGer	Abstract The CME’s structure of solar wind (interplanetary magnetic field) is different from CIR’s. The two processes in which plasma and solar wind energy are injected into the Earth’s inner magnetosphere are not the same. So, the variations of energetic electrons flux in the radiation belts are different between the storms associated with CMEs and CIRs. By using data from SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer) satellite, we have investigated the dynamic variations of the outer radiation belt for 1.5–6.0 MeV electrons during 54 CME-driven storms and 26 CIR-driven recurrent storms. According to the superposed epoch analysis, for CME- and CIR-driven storms, when the Dst index reaches the minimum, the locations of the outer boundary move to L=4 and L=5.5, respectively. In the recovery phases, the locations of the outer boundary of the outer radiation belt are generally lower than and slightly higher than those before CME- and CIR-driven storms, respectively. We have found that the logarithmically decaying 1/e cut-off L-shell is a satisfying indicator of the outer boundary of the outer radiation belt. Furthermore, our study shows that the logarithmically decaying 1/e cut-off latitude is dependent on the Kp index in the main phases of CME- and CIR- driven storms, while in the recovery phases, there is no obvious correlation. In addition, it has been shown that the locations of the peak electron flux are controlled by the minimum Dst index in the main phases of CME-driven storms. The influences of multiple storms on the electron flux of outer radiation belt have also been investigated.
abstract_unstemmed	Abstract The CME’s structure of solar wind (interplanetary magnetic field) is different from CIR’s. The two processes in which plasma and solar wind energy are injected into the Earth’s inner magnetosphere are not the same. So, the variations of energetic electrons flux in the radiation belts are different between the storms associated with CMEs and CIRs. By using data from SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer) satellite, we have investigated the dynamic variations of the outer radiation belt for 1.5–6.0 MeV electrons during 54 CME-driven storms and 26 CIR-driven recurrent storms. According to the superposed epoch analysis, for CME- and CIR-driven storms, when the Dst index reaches the minimum, the locations of the outer boundary move to L=4 and L=5.5, respectively. In the recovery phases, the locations of the outer boundary of the outer radiation belt are generally lower than and slightly higher than those before CME- and CIR-driven storms, respectively. We have found that the logarithmically decaying 1/e cut-off L-shell is a satisfying indicator of the outer boundary of the outer radiation belt. Furthermore, our study shows that the logarithmically decaying 1/e cut-off latitude is dependent on the Kp index in the main phases of CME- and CIR- driven storms, while in the recovery phases, there is no obvious correlation. In addition, it has been shown that the locations of the peak electron flux are controlled by the minimum Dst index in the main phases of CME-driven storms. The influences of multiple storms on the electron flux of outer radiation belt have also been investigated.
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title_short	Dynamic variations of the outer radiation belt during magnetic storms for 1.5–6.0 MeV electrons
url	https://dx.doi.org/10.1007/s11431-010-4269-9
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score	7.3988514

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Dynamic variations of the outer radiation belt during magnetic storms for 1.5–6.0 MeV electrons

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