Remote sensing of the proton aurora characteristics from IMAGE-FUV

The combination of simultaneous global images of the north polar region obtained with the IMAGE-FUV imaging system makes it possible to globally map the properties of the electron and proton auroral precipitation. The SI12 imager, which observes the Doppler-shifted Lyman-<font face="Symbol&q...
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Autor*in:	D. V. Bisikalo [verfasserIn] V. I. Shematovich [verfasserIn] J.-C. Gérard [verfasserIn] M. Meurant [verfasserIn] S. B. Mende [verfasserIn] H. U. Frey [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2003

Übergeordnetes Werk:	In: Annales Geophysicae - Copernicus Publications, 2002, 21(2003), Seite 2165-2173
Übergeordnetes Werk:	volume:21 ; year:2003 ; pages:2165-2173

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc Journal toc

DOI / URN:	10.5194/angeo-21-2165-2003

Katalog-ID:	DOAJ056384122

Internformat


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520			\|a The combination of simultaneous global images of the north polar region obtained with the IMAGE-FUV imaging system makes it possible to globally map the properties of the electron and proton auroral precipitation. The SI12 imager, which observes the Doppler-shifted Lyman-<font face="Symbol"<a</font< emission, provides a global snapshot of the proton aurora every 2 min. These images may be combined with those from the Wide-band Imaging Camera (WIC), to remotely characterize the proton precipitation in proton-dominated auroral structures frequently observed in the afternoon and pre-midnight sectors at the equatorial edge of the auroral oval. It is shown that both the proton energy flux and the mean energy determined by this method are in good agreement with coincident in situ measurement from low altitude satellites carrying proton detectors, when taking into account the different spatial resolution of the two types of observations. Four proton-dominated cases are illustrated in this study. They belong to two categories of proton auroral features: (i) hydrogen arcs known to occur in the evening sector equatorward of the electron oval and (ii) detached proton arcs observed with IMAGE-FUV in the afternoon sector following changes in orientation of the interplanetary magnetic field. They are characterized by a proton flux of 0.5–2 mWm<sup<-2</sup< and a mean energy in the range 10–17 keV.<br<<br<<b<Key words. </b<Magnetospheric physics (auroral phenomena; energetic particles, precipitating; magnetopause, cusp, arid boundary layers)
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spelling	10.5194/angeo-21-2165-2003 doi (DE-627)DOAJ056384122 (DE-599)DOAJb4dda38a9b034e9bbe3ce80ef195b6dc DE-627 ger DE-627 rakwb eng QC1-999 QC801-809 D. V. Bisikalo verfasserin aut Remote sensing of the proton aurora characteristics from IMAGE-FUV 2003 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier The combination of simultaneous global images of the north polar region obtained with the IMAGE-FUV imaging system makes it possible to globally map the properties of the electron and proton auroral precipitation. The SI12 imager, which observes the Doppler-shifted Lyman-<font face="Symbol"<a</font< emission, provides a global snapshot of the proton aurora every 2 min. These images may be combined with those from the Wide-band Imaging Camera (WIC), to remotely characterize the proton precipitation in proton-dominated auroral structures frequently observed in the afternoon and pre-midnight sectors at the equatorial edge of the auroral oval. It is shown that both the proton energy flux and the mean energy determined by this method are in good agreement with coincident in situ measurement from low altitude satellites carrying proton detectors, when taking into account the different spatial resolution of the two types of observations. Four proton-dominated cases are illustrated in this study. They belong to two categories of proton auroral features: (i) hydrogen arcs known to occur in the evening sector equatorward of the electron oval and (ii) detached proton arcs observed with IMAGE-FUV in the afternoon sector following changes in orientation of the interplanetary magnetic field. They are characterized by a proton flux of 0.5–2 mWm<sup<-2</sup< and a mean energy in the range 10–17 keV.<br<<br<<b<Key words. </b<Magnetospheric physics (auroral phenomena; energetic particles, precipitating; magnetopause, cusp, arid boundary layers) Science Q Physics Geophysics. Cosmic physics V. I. Shematovich verfasserin aut J.-C. Gérard verfasserin aut M. Meurant verfasserin aut S. B. Mende verfasserin aut H. U. Frey verfasserin aut In Annales Geophysicae Copernicus Publications, 2002 21(2003), Seite 2165-2173 (DE-627)25338981X (DE-600)1458425-6 14320576 nnns volume:21 year:2003 pages:2165-2173 https://doi.org/10.5194/angeo-21-2165-2003 kostenfrei https://doaj.org/article/b4dda38a9b034e9bbe3ce80ef195b6dc kostenfrei https://www.ann-geophys.net/21/2165/2003/angeo-21-2165-2003.pdf kostenfrei https://doaj.org/toc/0992-7689 Journal toc kostenfrei https://doaj.org/toc/1432-0576 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_267 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_381 GBV_ILN_602 GBV_ILN_2003 GBV_ILN_2014 GBV_ILN_2048 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 21 2003 2165-2173
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allfieldsGer	10.5194/angeo-21-2165-2003 doi (DE-627)DOAJ056384122 (DE-599)DOAJb4dda38a9b034e9bbe3ce80ef195b6dc DE-627 ger DE-627 rakwb eng QC1-999 QC801-809 D. V. Bisikalo verfasserin aut Remote sensing of the proton aurora characteristics from IMAGE-FUV 2003 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier The combination of simultaneous global images of the north polar region obtained with the IMAGE-FUV imaging system makes it possible to globally map the properties of the electron and proton auroral precipitation. The SI12 imager, which observes the Doppler-shifted Lyman-<font face="Symbol"<a</font< emission, provides a global snapshot of the proton aurora every 2 min. These images may be combined with those from the Wide-band Imaging Camera (WIC), to remotely characterize the proton precipitation in proton-dominated auroral structures frequently observed in the afternoon and pre-midnight sectors at the equatorial edge of the auroral oval. It is shown that both the proton energy flux and the mean energy determined by this method are in good agreement with coincident in situ measurement from low altitude satellites carrying proton detectors, when taking into account the different spatial resolution of the two types of observations. Four proton-dominated cases are illustrated in this study. They belong to two categories of proton auroral features: (i) hydrogen arcs known to occur in the evening sector equatorward of the electron oval and (ii) detached proton arcs observed with IMAGE-FUV in the afternoon sector following changes in orientation of the interplanetary magnetic field. They are characterized by a proton flux of 0.5–2 mWm<sup<-2</sup< and a mean energy in the range 10–17 keV.<br<<br<<b<Key words. </b<Magnetospheric physics (auroral phenomena; energetic particles, precipitating; magnetopause, cusp, arid boundary layers) Science Q Physics Geophysics. Cosmic physics V. I. Shematovich verfasserin aut J.-C. Gérard verfasserin aut M. Meurant verfasserin aut S. B. Mende verfasserin aut H. U. Frey verfasserin aut In Annales Geophysicae Copernicus Publications, 2002 21(2003), Seite 2165-2173 (DE-627)25338981X (DE-600)1458425-6 14320576 nnns volume:21 year:2003 pages:2165-2173 https://doi.org/10.5194/angeo-21-2165-2003 kostenfrei https://doaj.org/article/b4dda38a9b034e9bbe3ce80ef195b6dc kostenfrei https://www.ann-geophys.net/21/2165/2003/angeo-21-2165-2003.pdf kostenfrei https://doaj.org/toc/0992-7689 Journal toc kostenfrei https://doaj.org/toc/1432-0576 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_267 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_381 GBV_ILN_602 GBV_ILN_2003 GBV_ILN_2014 GBV_ILN_2048 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 21 2003 2165-2173
allfieldsSound	10.5194/angeo-21-2165-2003 doi (DE-627)DOAJ056384122 (DE-599)DOAJb4dda38a9b034e9bbe3ce80ef195b6dc DE-627 ger DE-627 rakwb eng QC1-999 QC801-809 D. V. Bisikalo verfasserin aut Remote sensing of the proton aurora characteristics from IMAGE-FUV 2003 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier The combination of simultaneous global images of the north polar region obtained with the IMAGE-FUV imaging system makes it possible to globally map the properties of the electron and proton auroral precipitation. The SI12 imager, which observes the Doppler-shifted Lyman-<font face="Symbol"<a</font< emission, provides a global snapshot of the proton aurora every 2 min. These images may be combined with those from the Wide-band Imaging Camera (WIC), to remotely characterize the proton precipitation in proton-dominated auroral structures frequently observed in the afternoon and pre-midnight sectors at the equatorial edge of the auroral oval. It is shown that both the proton energy flux and the mean energy determined by this method are in good agreement with coincident in situ measurement from low altitude satellites carrying proton detectors, when taking into account the different spatial resolution of the two types of observations. Four proton-dominated cases are illustrated in this study. They belong to two categories of proton auroral features: (i) hydrogen arcs known to occur in the evening sector equatorward of the electron oval and (ii) detached proton arcs observed with IMAGE-FUV in the afternoon sector following changes in orientation of the interplanetary magnetic field. They are characterized by a proton flux of 0.5–2 mWm<sup<-2</sup< and a mean energy in the range 10–17 keV.<br<<br<<b<Key words. </b<Magnetospheric physics (auroral phenomena; energetic particles, precipitating; magnetopause, cusp, arid boundary layers) Science Q Physics Geophysics. Cosmic physics V. I. Shematovich verfasserin aut J.-C. Gérard verfasserin aut M. Meurant verfasserin aut S. B. Mende verfasserin aut H. U. Frey verfasserin aut In Annales Geophysicae Copernicus Publications, 2002 21(2003), Seite 2165-2173 (DE-627)25338981X (DE-600)1458425-6 14320576 nnns volume:21 year:2003 pages:2165-2173 https://doi.org/10.5194/angeo-21-2165-2003 kostenfrei https://doaj.org/article/b4dda38a9b034e9bbe3ce80ef195b6dc kostenfrei https://www.ann-geophys.net/21/2165/2003/angeo-21-2165-2003.pdf kostenfrei https://doaj.org/toc/0992-7689 Journal toc kostenfrei https://doaj.org/toc/1432-0576 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_267 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_381 GBV_ILN_602 GBV_ILN_2003 GBV_ILN_2014 GBV_ILN_2048 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 21 2003 2165-2173
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callnumber-first	Q - Science
author	D. V. Bisikalo
spellingShingle	D. V. Bisikalo misc QC1-999 misc QC801-809 misc Science misc Q misc Physics misc Geophysics. Cosmic physics Remote sensing of the proton aurora characteristics from IMAGE-FUV
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topic_title	QC1-999 QC801-809 Remote sensing of the proton aurora characteristics from IMAGE-FUV
topic	misc QC1-999 misc QC801-809 misc Science misc Q misc Physics misc Geophysics. Cosmic physics
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title	Remote sensing of the proton aurora characteristics from IMAGE-FUV
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title_full	Remote sensing of the proton aurora characteristics from IMAGE-FUV
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title_sort	remote sensing of the proton aurora characteristics from image-fuv
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title_auth	Remote sensing of the proton aurora characteristics from IMAGE-FUV
abstract	The combination of simultaneous global images of the north polar region obtained with the IMAGE-FUV imaging system makes it possible to globally map the properties of the electron and proton auroral precipitation. The SI12 imager, which observes the Doppler-shifted Lyman-<font face="Symbol"<a</font< emission, provides a global snapshot of the proton aurora every 2 min. These images may be combined with those from the Wide-band Imaging Camera (WIC), to remotely characterize the proton precipitation in proton-dominated auroral structures frequently observed in the afternoon and pre-midnight sectors at the equatorial edge of the auroral oval. It is shown that both the proton energy flux and the mean energy determined by this method are in good agreement with coincident in situ measurement from low altitude satellites carrying proton detectors, when taking into account the different spatial resolution of the two types of observations. Four proton-dominated cases are illustrated in this study. They belong to two categories of proton auroral features: (i) hydrogen arcs known to occur in the evening sector equatorward of the electron oval and (ii) detached proton arcs observed with IMAGE-FUV in the afternoon sector following changes in orientation of the interplanetary magnetic field. They are characterized by a proton flux of 0.5–2 mWm<sup<-2</sup< and a mean energy in the range 10–17 keV.<br<<br<<b<Key words. </b<Magnetospheric physics (auroral phenomena; energetic particles, precipitating; magnetopause, cusp, arid boundary layers)
abstractGer	The combination of simultaneous global images of the north polar region obtained with the IMAGE-FUV imaging system makes it possible to globally map the properties of the electron and proton auroral precipitation. The SI12 imager, which observes the Doppler-shifted Lyman-<font face="Symbol"<a</font< emission, provides a global snapshot of the proton aurora every 2 min. These images may be combined with those from the Wide-band Imaging Camera (WIC), to remotely characterize the proton precipitation in proton-dominated auroral structures frequently observed in the afternoon and pre-midnight sectors at the equatorial edge of the auroral oval. It is shown that both the proton energy flux and the mean energy determined by this method are in good agreement with coincident in situ measurement from low altitude satellites carrying proton detectors, when taking into account the different spatial resolution of the two types of observations. Four proton-dominated cases are illustrated in this study. They belong to two categories of proton auroral features: (i) hydrogen arcs known to occur in the evening sector equatorward of the electron oval and (ii) detached proton arcs observed with IMAGE-FUV in the afternoon sector following changes in orientation of the interplanetary magnetic field. They are characterized by a proton flux of 0.5–2 mWm<sup<-2</sup< and a mean energy in the range 10–17 keV.<br<<br<<b<Key words. </b<Magnetospheric physics (auroral phenomena; energetic particles, precipitating; magnetopause, cusp, arid boundary layers)
abstract_unstemmed	The combination of simultaneous global images of the north polar region obtained with the IMAGE-FUV imaging system makes it possible to globally map the properties of the electron and proton auroral precipitation. The SI12 imager, which observes the Doppler-shifted Lyman-<font face="Symbol"<a</font< emission, provides a global snapshot of the proton aurora every 2 min. These images may be combined with those from the Wide-band Imaging Camera (WIC), to remotely characterize the proton precipitation in proton-dominated auroral structures frequently observed in the afternoon and pre-midnight sectors at the equatorial edge of the auroral oval. It is shown that both the proton energy flux and the mean energy determined by this method are in good agreement with coincident in situ measurement from low altitude satellites carrying proton detectors, when taking into account the different spatial resolution of the two types of observations. Four proton-dominated cases are illustrated in this study. They belong to two categories of proton auroral features: (i) hydrogen arcs known to occur in the evening sector equatorward of the electron oval and (ii) detached proton arcs observed with IMAGE-FUV in the afternoon sector following changes in orientation of the interplanetary magnetic field. They are characterized by a proton flux of 0.5–2 mWm<sup<-2</sup< and a mean energy in the range 10–17 keV.<br<<br<<b<Key words. </b<Magnetospheric physics (auroral phenomena; energetic particles, precipitating; magnetopause, cusp, arid boundary layers)
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title_short	Remote sensing of the proton aurora characteristics from IMAGE-FUV
url	https://doi.org/10.5194/angeo-21-2165-2003 https://doaj.org/article/b4dda38a9b034e9bbe3ce80ef195b6dc https://www.ann-geophys.net/21/2165/2003/angeo-21-2165-2003.pdf https://doaj.org/toc/0992-7689 https://doaj.org/toc/1432-0576
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up_date	2024-07-03T20:31:56.109Z
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They belong to two categories of proton auroral features: (i) hydrogen arcs known to occur in the evening sector equatorward of the electron oval and (ii) detached proton arcs observed with IMAGE-FUV in the afternoon sector following changes in orientation of the interplanetary magnetic field. They are characterized by a proton flux of 0.5–2 mWm<sup<-2</sup< and a mean energy in the range 10–17 keV.<br<<br<<b<Key words. </b<Magnetospheric physics (auroral phenomena; energetic particles, precipitating; magnetopause, cusp, arid boundary layers)</subfield></datafield><datafield tag="653" ind1=" " ind2="0"><subfield code="a">Science</subfield></datafield><datafield tag="653" ind1=" " ind2="0"><subfield code="a">Q</subfield></datafield><datafield tag="653" ind1=" " ind2="0"><subfield code="a">Physics</subfield></datafield><datafield tag="653" ind1=" " ind2="0"><subfield code="a">Geophysics. Cosmic physics</subfield></datafield><datafield tag="700" ind1="0" ind2=" "><subfield code="a">V. I. 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Remote sensing of the proton aurora characteristics from IMAGE-FUV

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