Response of the magnetic field and plasmas at the geosynchronous orbit to interplanetary shock

Abstract Interplanetary shock can greatly disturb the Earth’s magnetosphere and ionosphere, causing the temporal and spatial changes of the magnetic field and plasmas at the geosynchronous orbit. In this paper, we use the magnetic field data of GOES satellites from 1997 to 2007 and the plasma data of MPA on the LANL satellites from 1997 to 2004 to study the properties of magnetic field and plasma (0.03–45 keV) at the geosynchronous orbit (6.6 RE) within 3 hours before and after the arrival of shock front at the geosynchronous orbit through both case study and superposed epoch analysis. It is found that following the arrival of shock front at the geosynchronous orbit, the magnetic field magnitude, as well as GSM BZ component increases significantly on the dayside (8–16 LT), while the BY component has almost no change before and after shock impacts. In response to the interplanetary shock, the proton becomes much denser with a peak number density of 1.2 $ cm^{−3} $, compared to the typical number density of 0.7 $ cm^{−3} $. The proton temperature increases sharply, predominantly on the dusk and night side. The electron, density increases dramatically on the night side with a peak number density of 2.0 $ cm^{−3} $. The inferred ionospheric $ O^{+} $ density after the interplanetary shock impact reaches the maximum value of 1.2 $ cm^{−3} $ on the dusk side and exhibits the clear dawn-dusk asymmetry. The peak of the anisotropy of proton’s temperature is located at the noon sector, and the anisotropy decreases towards the dawn and dusk side. The minimum of temperature anisotropy is on the night side. It is suggested that the electromagnetic ion cyclotron (EMIC) wave and whistler wave can be stimulated by the proton and electron temperature anisotropy respectively. The computed electromagnetic ion cyclotron wave (EMIC) intense on the day side (8–16 LT) with a frequency value of 0.8 Hz, and the wave intensity decreases towards the dawn and dusk side, the minimum value can be found on the night side. The computed electron whistler wave locates on the day side (8–16 LT) with a value of 2 kHz. Ausführliche Beschreibung

Gespeichert in:

Autor*in:	Yue, Chao [verfasserIn] Zong, QiuGang [verfasserIn] Wang, YongFu [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2009

Schlagwörter:	interplanetary shock geosynchronous orbit superposed epoch analysis electromagnetic ion cyclotron wave whistler wave

Übergeordnetes Werk:	Enthalten in: Chinese science bulletin - Beijing, China : Chinese Acad. of Sciences, 1997, 54(2009), 22 vom: 10. Dez.
Übergeordnetes Werk:	volume:54 ; year:2009 ; number:22 ; day:10 ; month:12

Links:	Volltext

DOI / URN:	10.1007/s11434-009-0649-6

Katalog-ID:	SPR019386303

Internformat


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520			\|a Abstract Interplanetary shock can greatly disturb the Earth’s magnetosphere and ionosphere, causing the temporal and spatial changes of the magnetic field and plasmas at the geosynchronous orbit. In this paper, we use the magnetic field data of GOES satellites from 1997 to 2007 and the plasma data of MPA on the LANL satellites from 1997 to 2004 to study the properties of magnetic field and plasma (0.03–45 keV) at the geosynchronous orbit (6.6 RE) within 3 hours before and after the arrival of shock front at the geosynchronous orbit through both case study and superposed epoch analysis. It is found that following the arrival of shock front at the geosynchronous orbit, the magnetic field magnitude, as well as GSM BZ component increases significantly on the dayside (8–16 LT), while the BY component has almost no change before and after shock impacts. In response to the interplanetary shock, the proton becomes much denser with a peak number density of 1.2 $ cm^{−3} $, compared to the typical number density of 0.7 $ cm^{−3} $. The proton temperature increases sharply, predominantly on the dusk and night side. The electron, density increases dramatically on the night side with a peak number density of 2.0 $ cm^{−3} $. The inferred ionospheric $ O^{+} $ density after the interplanetary shock impact reaches the maximum value of 1.2 $ cm^{−3} $ on the dusk side and exhibits the clear dawn-dusk asymmetry. The peak of the anisotropy of proton’s temperature is located at the noon sector, and the anisotropy decreases towards the dawn and dusk side. The minimum of temperature anisotropy is on the night side. It is suggested that the electromagnetic ion cyclotron (EMIC) wave and whistler wave can be stimulated by the proton and electron temperature anisotropy respectively. The computed electromagnetic ion cyclotron wave (EMIC) intense on the day side (8–16 LT) with a frequency value of 0.8 Hz, and the wave intensity decreases towards the dawn and dusk side, the minimum value can be found on the night side. The computed electron whistler wave locates on the day side (8–16 LT) with a value of 2 kHz.
650		4	\|a interplanetary shock \|7 (dpeaa)DE-He213
650		4	\|a geosynchronous orbit \|7 (dpeaa)DE-He213
650		4	\|a superposed epoch analysis \|7 (dpeaa)DE-He213
650		4	\|a electromagnetic ion cyclotron wave \|7 (dpeaa)DE-He213
650		4	\|a whistler wave \|7 (dpeaa)DE-He213
700	1		\|a Zong, QiuGang \|e verfasserin \|4 aut
700	1		\|a Wang, YongFu \|e verfasserin \|4 aut
773	0	8	\|i Enthalten in \|t Chinese science bulletin \|d Beijing, China : Chinese Acad. of Sciences, 1997 \|g 54(2009), 22 vom: 10. Dez. \|w (DE-627)341897809 \|w (DE-600)2069521-4 \|x 1861-9541 \|7 nnns
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936	b	k	\|a 30.00 \|q ASE
951			\|a AR
952			\|d 54 \|j 2009 \|e 22 \|b 10 \|c 12

Indexfelder

author_variant	c y cy q z qz y w yw
matchkey_str	article:18619541:2009----::epnefhmgeifednpamsthgoycrnuobt
hierarchy_sort_str	2009
bklnumber	30.00
publishDate	2009
allfields	10.1007/s11434-009-0649-6 doi (DE-627)SPR019386303 (SPR)s11434-009-0649-6-e DE-627 ger DE-627 rakwb eng 500 ASE 30.00 bkl Yue, Chao verfasserin aut Response of the magnetic field and plasmas at the geosynchronous orbit to interplanetary shock 2009 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract Interplanetary shock can greatly disturb the Earth’s magnetosphere and ionosphere, causing the temporal and spatial changes of the magnetic field and plasmas at the geosynchronous orbit. In this paper, we use the magnetic field data of GOES satellites from 1997 to 2007 and the plasma data of MPA on the LANL satellites from 1997 to 2004 to study the properties of magnetic field and plasma (0.03–45 keV) at the geosynchronous orbit (6.6 RE) within 3 hours before and after the arrival of shock front at the geosynchronous orbit through both case study and superposed epoch analysis. It is found that following the arrival of shock front at the geosynchronous orbit, the magnetic field magnitude, as well as GSM BZ component increases significantly on the dayside (8–16 LT), while the BY component has almost no change before and after shock impacts. In response to the interplanetary shock, the proton becomes much denser with a peak number density of 1.2 $ cm^{−3} $, compared to the typical number density of 0.7 $ cm^{−3} $. The proton temperature increases sharply, predominantly on the dusk and night side. The electron, density increases dramatically on the night side with a peak number density of 2.0 $ cm^{−3} $. The inferred ionospheric $ O^{+} $ density after the interplanetary shock impact reaches the maximum value of 1.2 $ cm^{−3} $ on the dusk side and exhibits the clear dawn-dusk asymmetry. The peak of the anisotropy of proton’s temperature is located at the noon sector, and the anisotropy decreases towards the dawn and dusk side. The minimum of temperature anisotropy is on the night side. It is suggested that the electromagnetic ion cyclotron (EMIC) wave and whistler wave can be stimulated by the proton and electron temperature anisotropy respectively. The computed electromagnetic ion cyclotron wave (EMIC) intense on the day side (8–16 LT) with a frequency value of 0.8 Hz, and the wave intensity decreases towards the dawn and dusk side, the minimum value can be found on the night side. The computed electron whistler wave locates on the day side (8–16 LT) with a value of 2 kHz. interplanetary shock (dpeaa)DE-He213 geosynchronous orbit (dpeaa)DE-He213 superposed epoch analysis (dpeaa)DE-He213 electromagnetic ion cyclotron wave (dpeaa)DE-He213 whistler wave (dpeaa)DE-He213 Zong, QiuGang verfasserin aut Wang, YongFu verfasserin aut Enthalten in Chinese science bulletin Beijing, China : Chinese Acad. of Sciences, 1997 54(2009), 22 vom: 10. Dez. (DE-627)341897809 (DE-600)2069521-4 1861-9541 nnns volume:54 year:2009 number:22 day:10 month:12 https://dx.doi.org/10.1007/s11434-009-0649-6 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_20 GBV_ILN_40 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_110 GBV_ILN_120 GBV_ILN_161 GBV_ILN_266 GBV_ILN_285 GBV_ILN_293 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2055 GBV_ILN_2059 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4313 GBV_ILN_4328 GBV_ILN_4333 30.00 ASE AR 54 2009 22 10 12
spelling	10.1007/s11434-009-0649-6 doi (DE-627)SPR019386303 (SPR)s11434-009-0649-6-e DE-627 ger DE-627 rakwb eng 500 ASE 30.00 bkl Yue, Chao verfasserin aut Response of the magnetic field and plasmas at the geosynchronous orbit to interplanetary shock 2009 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract Interplanetary shock can greatly disturb the Earth’s magnetosphere and ionosphere, causing the temporal and spatial changes of the magnetic field and plasmas at the geosynchronous orbit. In this paper, we use the magnetic field data of GOES satellites from 1997 to 2007 and the plasma data of MPA on the LANL satellites from 1997 to 2004 to study the properties of magnetic field and plasma (0.03–45 keV) at the geosynchronous orbit (6.6 RE) within 3 hours before and after the arrival of shock front at the geosynchronous orbit through both case study and superposed epoch analysis. It is found that following the arrival of shock front at the geosynchronous orbit, the magnetic field magnitude, as well as GSM BZ component increases significantly on the dayside (8–16 LT), while the BY component has almost no change before and after shock impacts. In response to the interplanetary shock, the proton becomes much denser with a peak number density of 1.2 $ cm^{−3} $, compared to the typical number density of 0.7 $ cm^{−3} $. The proton temperature increases sharply, predominantly on the dusk and night side. The electron, density increases dramatically on the night side with a peak number density of 2.0 $ cm^{−3} $. The inferred ionospheric $ O^{+} $ density after the interplanetary shock impact reaches the maximum value of 1.2 $ cm^{−3} $ on the dusk side and exhibits the clear dawn-dusk asymmetry. The peak of the anisotropy of proton’s temperature is located at the noon sector, and the anisotropy decreases towards the dawn and dusk side. The minimum of temperature anisotropy is on the night side. It is suggested that the electromagnetic ion cyclotron (EMIC) wave and whistler wave can be stimulated by the proton and electron temperature anisotropy respectively. The computed electromagnetic ion cyclotron wave (EMIC) intense on the day side (8–16 LT) with a frequency value of 0.8 Hz, and the wave intensity decreases towards the dawn and dusk side, the minimum value can be found on the night side. The computed electron whistler wave locates on the day side (8–16 LT) with a value of 2 kHz. interplanetary shock (dpeaa)DE-He213 geosynchronous orbit (dpeaa)DE-He213 superposed epoch analysis (dpeaa)DE-He213 electromagnetic ion cyclotron wave (dpeaa)DE-He213 whistler wave (dpeaa)DE-He213 Zong, QiuGang verfasserin aut Wang, YongFu verfasserin aut Enthalten in Chinese science bulletin Beijing, China : Chinese Acad. of Sciences, 1997 54(2009), 22 vom: 10. Dez. (DE-627)341897809 (DE-600)2069521-4 1861-9541 nnns volume:54 year:2009 number:22 day:10 month:12 https://dx.doi.org/10.1007/s11434-009-0649-6 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_20 GBV_ILN_40 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_110 GBV_ILN_120 GBV_ILN_161 GBV_ILN_266 GBV_ILN_285 GBV_ILN_293 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2055 GBV_ILN_2059 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4313 GBV_ILN_4328 GBV_ILN_4333 30.00 ASE AR 54 2009 22 10 12
allfields_unstemmed	10.1007/s11434-009-0649-6 doi (DE-627)SPR019386303 (SPR)s11434-009-0649-6-e DE-627 ger DE-627 rakwb eng 500 ASE 30.00 bkl Yue, Chao verfasserin aut Response of the magnetic field and plasmas at the geosynchronous orbit to interplanetary shock 2009 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract Interplanetary shock can greatly disturb the Earth’s magnetosphere and ionosphere, causing the temporal and spatial changes of the magnetic field and plasmas at the geosynchronous orbit. In this paper, we use the magnetic field data of GOES satellites from 1997 to 2007 and the plasma data of MPA on the LANL satellites from 1997 to 2004 to study the properties of magnetic field and plasma (0.03–45 keV) at the geosynchronous orbit (6.6 RE) within 3 hours before and after the arrival of shock front at the geosynchronous orbit through both case study and superposed epoch analysis. It is found that following the arrival of shock front at the geosynchronous orbit, the magnetic field magnitude, as well as GSM BZ component increases significantly on the dayside (8–16 LT), while the BY component has almost no change before and after shock impacts. In response to the interplanetary shock, the proton becomes much denser with a peak number density of 1.2 $ cm^{−3} $, compared to the typical number density of 0.7 $ cm^{−3} $. The proton temperature increases sharply, predominantly on the dusk and night side. The electron, density increases dramatically on the night side with a peak number density of 2.0 $ cm^{−3} $. The inferred ionospheric $ O^{+} $ density after the interplanetary shock impact reaches the maximum value of 1.2 $ cm^{−3} $ on the dusk side and exhibits the clear dawn-dusk asymmetry. The peak of the anisotropy of proton’s temperature is located at the noon sector, and the anisotropy decreases towards the dawn and dusk side. The minimum of temperature anisotropy is on the night side. It is suggested that the electromagnetic ion cyclotron (EMIC) wave and whistler wave can be stimulated by the proton and electron temperature anisotropy respectively. The computed electromagnetic ion cyclotron wave (EMIC) intense on the day side (8–16 LT) with a frequency value of 0.8 Hz, and the wave intensity decreases towards the dawn and dusk side, the minimum value can be found on the night side. The computed electron whistler wave locates on the day side (8–16 LT) with a value of 2 kHz. interplanetary shock (dpeaa)DE-He213 geosynchronous orbit (dpeaa)DE-He213 superposed epoch analysis (dpeaa)DE-He213 electromagnetic ion cyclotron wave (dpeaa)DE-He213 whistler wave (dpeaa)DE-He213 Zong, QiuGang verfasserin aut Wang, YongFu verfasserin aut Enthalten in Chinese science bulletin Beijing, China : Chinese Acad. of Sciences, 1997 54(2009), 22 vom: 10. Dez. (DE-627)341897809 (DE-600)2069521-4 1861-9541 nnns volume:54 year:2009 number:22 day:10 month:12 https://dx.doi.org/10.1007/s11434-009-0649-6 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_20 GBV_ILN_40 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_110 GBV_ILN_120 GBV_ILN_161 GBV_ILN_266 GBV_ILN_285 GBV_ILN_293 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2055 GBV_ILN_2059 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4313 GBV_ILN_4328 GBV_ILN_4333 30.00 ASE AR 54 2009 22 10 12
allfieldsGer	10.1007/s11434-009-0649-6 doi (DE-627)SPR019386303 (SPR)s11434-009-0649-6-e DE-627 ger DE-627 rakwb eng 500 ASE 30.00 bkl Yue, Chao verfasserin aut Response of the magnetic field and plasmas at the geosynchronous orbit to interplanetary shock 2009 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract Interplanetary shock can greatly disturb the Earth’s magnetosphere and ionosphere, causing the temporal and spatial changes of the magnetic field and plasmas at the geosynchronous orbit. In this paper, we use the magnetic field data of GOES satellites from 1997 to 2007 and the plasma data of MPA on the LANL satellites from 1997 to 2004 to study the properties of magnetic field and plasma (0.03–45 keV) at the geosynchronous orbit (6.6 RE) within 3 hours before and after the arrival of shock front at the geosynchronous orbit through both case study and superposed epoch analysis. It is found that following the arrival of shock front at the geosynchronous orbit, the magnetic field magnitude, as well as GSM BZ component increases significantly on the dayside (8–16 LT), while the BY component has almost no change before and after shock impacts. In response to the interplanetary shock, the proton becomes much denser with a peak number density of 1.2 $ cm^{−3} $, compared to the typical number density of 0.7 $ cm^{−3} $. The proton temperature increases sharply, predominantly on the dusk and night side. The electron, density increases dramatically on the night side with a peak number density of 2.0 $ cm^{−3} $. The inferred ionospheric $ O^{+} $ density after the interplanetary shock impact reaches the maximum value of 1.2 $ cm^{−3} $ on the dusk side and exhibits the clear dawn-dusk asymmetry. The peak of the anisotropy of proton’s temperature is located at the noon sector, and the anisotropy decreases towards the dawn and dusk side. The minimum of temperature anisotropy is on the night side. It is suggested that the electromagnetic ion cyclotron (EMIC) wave and whistler wave can be stimulated by the proton and electron temperature anisotropy respectively. The computed electromagnetic ion cyclotron wave (EMIC) intense on the day side (8–16 LT) with a frequency value of 0.8 Hz, and the wave intensity decreases towards the dawn and dusk side, the minimum value can be found on the night side. The computed electron whistler wave locates on the day side (8–16 LT) with a value of 2 kHz. interplanetary shock (dpeaa)DE-He213 geosynchronous orbit (dpeaa)DE-He213 superposed epoch analysis (dpeaa)DE-He213 electromagnetic ion cyclotron wave (dpeaa)DE-He213 whistler wave (dpeaa)DE-He213 Zong, QiuGang verfasserin aut Wang, YongFu verfasserin aut Enthalten in Chinese science bulletin Beijing, China : Chinese Acad. of Sciences, 1997 54(2009), 22 vom: 10. Dez. (DE-627)341897809 (DE-600)2069521-4 1861-9541 nnns volume:54 year:2009 number:22 day:10 month:12 https://dx.doi.org/10.1007/s11434-009-0649-6 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_20 GBV_ILN_40 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_110 GBV_ILN_120 GBV_ILN_161 GBV_ILN_266 GBV_ILN_285 GBV_ILN_293 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2055 GBV_ILN_2059 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4313 GBV_ILN_4328 GBV_ILN_4333 30.00 ASE AR 54 2009 22 10 12
allfieldsSound	10.1007/s11434-009-0649-6 doi (DE-627)SPR019386303 (SPR)s11434-009-0649-6-e DE-627 ger DE-627 rakwb eng 500 ASE 30.00 bkl Yue, Chao verfasserin aut Response of the magnetic field and plasmas at the geosynchronous orbit to interplanetary shock 2009 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract Interplanetary shock can greatly disturb the Earth’s magnetosphere and ionosphere, causing the temporal and spatial changes of the magnetic field and plasmas at the geosynchronous orbit. In this paper, we use the magnetic field data of GOES satellites from 1997 to 2007 and the plasma data of MPA on the LANL satellites from 1997 to 2004 to study the properties of magnetic field and plasma (0.03–45 keV) at the geosynchronous orbit (6.6 RE) within 3 hours before and after the arrival of shock front at the geosynchronous orbit through both case study and superposed epoch analysis. It is found that following the arrival of shock front at the geosynchronous orbit, the magnetic field magnitude, as well as GSM BZ component increases significantly on the dayside (8–16 LT), while the BY component has almost no change before and after shock impacts. In response to the interplanetary shock, the proton becomes much denser with a peak number density of 1.2 $ cm^{−3} $, compared to the typical number density of 0.7 $ cm^{−3} $. The proton temperature increases sharply, predominantly on the dusk and night side. The electron, density increases dramatically on the night side with a peak number density of 2.0 $ cm^{−3} $. The inferred ionospheric $ O^{+} $ density after the interplanetary shock impact reaches the maximum value of 1.2 $ cm^{−3} $ on the dusk side and exhibits the clear dawn-dusk asymmetry. The peak of the anisotropy of proton’s temperature is located at the noon sector, and the anisotropy decreases towards the dawn and dusk side. The minimum of temperature anisotropy is on the night side. It is suggested that the electromagnetic ion cyclotron (EMIC) wave and whistler wave can be stimulated by the proton and electron temperature anisotropy respectively. The computed electromagnetic ion cyclotron wave (EMIC) intense on the day side (8–16 LT) with a frequency value of 0.8 Hz, and the wave intensity decreases towards the dawn and dusk side, the minimum value can be found on the night side. The computed electron whistler wave locates on the day side (8–16 LT) with a value of 2 kHz. interplanetary shock (dpeaa)DE-He213 geosynchronous orbit (dpeaa)DE-He213 superposed epoch analysis (dpeaa)DE-He213 electromagnetic ion cyclotron wave (dpeaa)DE-He213 whistler wave (dpeaa)DE-He213 Zong, QiuGang verfasserin aut Wang, YongFu verfasserin aut Enthalten in Chinese science bulletin Beijing, China : Chinese Acad. of Sciences, 1997 54(2009), 22 vom: 10. Dez. (DE-627)341897809 (DE-600)2069521-4 1861-9541 nnns volume:54 year:2009 number:22 day:10 month:12 https://dx.doi.org/10.1007/s11434-009-0649-6 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_20 GBV_ILN_40 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_110 GBV_ILN_120 GBV_ILN_161 GBV_ILN_266 GBV_ILN_285 GBV_ILN_293 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2018 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2055 GBV_ILN_2059 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4313 GBV_ILN_4328 GBV_ILN_4333 30.00 ASE AR 54 2009 22 10 12
language	English
source	Enthalten in Chinese science bulletin 54(2009), 22 vom: 10. Dez. volume:54 year:2009 number:22 day:10 month:12
sourceStr	Enthalten in Chinese science bulletin 54(2009), 22 vom: 10. Dez. volume:54 year:2009 number:22 day:10 month:12
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	interplanetary shock geosynchronous orbit superposed epoch analysis electromagnetic ion cyclotron wave whistler wave
dewey-raw	500
isfreeaccess_bool	false
container_title	Chinese science bulletin
authorswithroles_txt_mv	Yue, Chao @@aut@@ Zong, QiuGang @@aut@@ Wang, YongFu @@aut@@
publishDateDaySort_date	2009-12-10T00:00:00Z
hierarchy_top_id	341897809
dewey-sort	3500
id	SPR019386303
language_de	englisch
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author	Yue, Chao
spellingShingle	Yue, Chao ddc 500 bkl 30.00 misc interplanetary shock misc geosynchronous orbit misc superposed epoch analysis misc electromagnetic ion cyclotron wave misc whistler wave Response of the magnetic field and plasmas at the geosynchronous orbit to interplanetary shock
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topic_title	500 ASE 30.00 bkl Response of the magnetic field and plasmas at the geosynchronous orbit to interplanetary shock interplanetary shock (dpeaa)DE-He213 geosynchronous orbit (dpeaa)DE-He213 superposed epoch analysis (dpeaa)DE-He213 electromagnetic ion cyclotron wave (dpeaa)DE-He213 whistler wave (dpeaa)DE-He213
topic	ddc 500 bkl 30.00 misc interplanetary shock misc geosynchronous orbit misc superposed epoch analysis misc electromagnetic ion cyclotron wave misc whistler wave
topic_unstemmed	ddc 500 bkl 30.00 misc interplanetary shock misc geosynchronous orbit misc superposed epoch analysis misc electromagnetic ion cyclotron wave misc whistler wave
topic_browse	ddc 500 bkl 30.00 misc interplanetary shock misc geosynchronous orbit misc superposed epoch analysis misc electromagnetic ion cyclotron wave misc whistler wave
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title	Response of the magnetic field and plasmas at the geosynchronous orbit to interplanetary shock
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title_full	Response of the magnetic field and plasmas at the geosynchronous orbit to interplanetary shock
author_sort	Yue, Chao
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author_browse	Yue, Chao Zong, QiuGang Wang, YongFu
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title_sort	response of the magnetic field and plasmas at the geosynchronous orbit to interplanetary shock
title_auth	Response of the magnetic field and plasmas at the geosynchronous orbit to interplanetary shock
abstract	Abstract Interplanetary shock can greatly disturb the Earth’s magnetosphere and ionosphere, causing the temporal and spatial changes of the magnetic field and plasmas at the geosynchronous orbit. In this paper, we use the magnetic field data of GOES satellites from 1997 to 2007 and the plasma data of MPA on the LANL satellites from 1997 to 2004 to study the properties of magnetic field and plasma (0.03–45 keV) at the geosynchronous orbit (6.6 RE) within 3 hours before and after the arrival of shock front at the geosynchronous orbit through both case study and superposed epoch analysis. It is found that following the arrival of shock front at the geosynchronous orbit, the magnetic field magnitude, as well as GSM BZ component increases significantly on the dayside (8–16 LT), while the BY component has almost no change before and after shock impacts. In response to the interplanetary shock, the proton becomes much denser with a peak number density of 1.2 $ cm^{−3} $, compared to the typical number density of 0.7 $ cm^{−3} $. The proton temperature increases sharply, predominantly on the dusk and night side. The electron, density increases dramatically on the night side with a peak number density of 2.0 $ cm^{−3} $. The inferred ionospheric $ O^{+} $ density after the interplanetary shock impact reaches the maximum value of 1.2 $ cm^{−3} $ on the dusk side and exhibits the clear dawn-dusk asymmetry. The peak of the anisotropy of proton’s temperature is located at the noon sector, and the anisotropy decreases towards the dawn and dusk side. The minimum of temperature anisotropy is on the night side. It is suggested that the electromagnetic ion cyclotron (EMIC) wave and whistler wave can be stimulated by the proton and electron temperature anisotropy respectively. The computed electromagnetic ion cyclotron wave (EMIC) intense on the day side (8–16 LT) with a frequency value of 0.8 Hz, and the wave intensity decreases towards the dawn and dusk side, the minimum value can be found on the night side. The computed electron whistler wave locates on the day side (8–16 LT) with a value of 2 kHz.
abstractGer	Abstract Interplanetary shock can greatly disturb the Earth’s magnetosphere and ionosphere, causing the temporal and spatial changes of the magnetic field and plasmas at the geosynchronous orbit. In this paper, we use the magnetic field data of GOES satellites from 1997 to 2007 and the plasma data of MPA on the LANL satellites from 1997 to 2004 to study the properties of magnetic field and plasma (0.03–45 keV) at the geosynchronous orbit (6.6 RE) within 3 hours before and after the arrival of shock front at the geosynchronous orbit through both case study and superposed epoch analysis. It is found that following the arrival of shock front at the geosynchronous orbit, the magnetic field magnitude, as well as GSM BZ component increases significantly on the dayside (8–16 LT), while the BY component has almost no change before and after shock impacts. In response to the interplanetary shock, the proton becomes much denser with a peak number density of 1.2 $ cm^{−3} $, compared to the typical number density of 0.7 $ cm^{−3} $. The proton temperature increases sharply, predominantly on the dusk and night side. The electron, density increases dramatically on the night side with a peak number density of 2.0 $ cm^{−3} $. The inferred ionospheric $ O^{+} $ density after the interplanetary shock impact reaches the maximum value of 1.2 $ cm^{−3} $ on the dusk side and exhibits the clear dawn-dusk asymmetry. The peak of the anisotropy of proton’s temperature is located at the noon sector, and the anisotropy decreases towards the dawn and dusk side. The minimum of temperature anisotropy is on the night side. It is suggested that the electromagnetic ion cyclotron (EMIC) wave and whistler wave can be stimulated by the proton and electron temperature anisotropy respectively. The computed electromagnetic ion cyclotron wave (EMIC) intense on the day side (8–16 LT) with a frequency value of 0.8 Hz, and the wave intensity decreases towards the dawn and dusk side, the minimum value can be found on the night side. The computed electron whistler wave locates on the day side (8–16 LT) with a value of 2 kHz.
abstract_unstemmed	Abstract Interplanetary shock can greatly disturb the Earth’s magnetosphere and ionosphere, causing the temporal and spatial changes of the magnetic field and plasmas at the geosynchronous orbit. In this paper, we use the magnetic field data of GOES satellites from 1997 to 2007 and the plasma data of MPA on the LANL satellites from 1997 to 2004 to study the properties of magnetic field and plasma (0.03–45 keV) at the geosynchronous orbit (6.6 RE) within 3 hours before and after the arrival of shock front at the geosynchronous orbit through both case study and superposed epoch analysis. It is found that following the arrival of shock front at the geosynchronous orbit, the magnetic field magnitude, as well as GSM BZ component increases significantly on the dayside (8–16 LT), while the BY component has almost no change before and after shock impacts. In response to the interplanetary shock, the proton becomes much denser with a peak number density of 1.2 $ cm^{−3} $, compared to the typical number density of 0.7 $ cm^{−3} $. The proton temperature increases sharply, predominantly on the dusk and night side. The electron, density increases dramatically on the night side with a peak number density of 2.0 $ cm^{−3} $. The inferred ionospheric $ O^{+} $ density after the interplanetary shock impact reaches the maximum value of 1.2 $ cm^{−3} $ on the dusk side and exhibits the clear dawn-dusk asymmetry. The peak of the anisotropy of proton’s temperature is located at the noon sector, and the anisotropy decreases towards the dawn and dusk side. The minimum of temperature anisotropy is on the night side. It is suggested that the electromagnetic ion cyclotron (EMIC) wave and whistler wave can be stimulated by the proton and electron temperature anisotropy respectively. The computed electromagnetic ion cyclotron wave (EMIC) intense on the day side (8–16 LT) with a frequency value of 0.8 Hz, and the wave intensity decreases towards the dawn and dusk side, the minimum value can be found on the night side. The computed electron whistler wave locates on the day side (8–16 LT) with a value of 2 kHz.
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title_short	Response of the magnetic field and plasmas at the geosynchronous orbit to interplanetary shock
url	https://dx.doi.org/10.1007/s11434-009-0649-6
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Response of the magnetic field and plasmas at the geosynchronous orbit to interplanetary shock

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