The effects of geomagnetic storms on electrons in Earth's radiation belts
We use Van Allen Probes data to investigate the responses of tens of keV to 2 MeV electrons throughout a broad range of the radiation belts (2.5 ≤ L ≤ 6.0) during 52 geomagnetic storms from the most recent solar maximum. Electron storm time responses are highly dependent on both electron energy an...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Turner, D. L [verfasserIn] |
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| Format: |
Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2015 |
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| Rechteinformationen: |
Nutzungsrecht: © 2015. American Geophysical Union. All Rights Reserved. |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
Enthalten in: Geophysical research letters - Washington, DC : Union, 1974, 42(2015), 21, Seite 9176-9184 |
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| Übergeordnetes Werk: |
volume:42 ; year:2015 ; number:21 ; pages:9176-9184 |
| Links: |
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| DOI / URN: |
10.1002/2015GL064747 |
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| 520 | |a We use Van Allen Probes data to investigate the responses of tens of keV to 2 MeV electrons throughout a broad range of the radiation belts (2.5 ≤ L ≤ 6.0) during 52 geomagnetic storms from the most recent solar maximum. Electron storm time responses are highly dependent on both electron energy and L shell. Tens of keV electrons typically have peak fluxes in the inner belt or near‐Earth plasma sheet and fill the inner magnetosphere during storm main phases. Approximately 100 to ~600 keV electrons are enhanced in up to 87% of cases around L ~3.7, and their peak flux location moves to lower L shells during storm recovery phases. Relativistic electrons (≥~1 MeV) are nearly equally likely to produce enhancement, depletion, and no‐change events in the outer belt. We also show that the L shell of peak flux correlates to storm magnitude only for hundreds of keV electrons. Near L~3.7, ~100 to ~600 keV electrons are enhanced during up to 87% of storm recovery phases Relativistic electrons are split between enhancement, depletion, and no‐change events For hundreds of keV electrons, peak flux L shell after the storm correlates well to storms' SYM‐H minima | ||
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| 650 | 4 | |a radiation belts | |
| 650 | 4 | |a geomagnetic storms | |
| 650 | 4 | |a electrons | |
| 650 | 4 | |a Electrons | |
| 650 | 4 | |a Earth | |
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| 700 | 1 | |a O'Brien, T. P |4 oth | |
| 700 | 1 | |a Fennell, J. F |4 oth | |
| 700 | 1 | |a Claudepierre, S. G |4 oth | |
| 700 | 1 | |a Blake, J. B |4 oth | |
| 700 | 1 | |a Kilpua, E. K. J |4 oth | |
| 700 | 1 | |a Hietala, H |4 oth | |
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10.1002/2015GL064747 doi PQ20160617 (DE-627)OLC1964143772 (DE-599)GBVOLC1964143772 (PRQ)p956-b03942ad5e0b98f6f86f5734b4d5b629552f5d76e7be3ea6087ab5fe7d146dfd0 (KEY)0026932820150000042002109176effectsofgeomagneticstormsonelectronsinearthsradia DE-627 ger DE-627 rakwb eng 550 DNB 38.70 bkl Turner, D. L verfasserin aut The effects of geomagnetic storms on electrons in Earth's radiation belts 2015 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier We use Van Allen Probes data to investigate the responses of tens of keV to 2 MeV electrons throughout a broad range of the radiation belts (2.5 ≤ L ≤ 6.0) during 52 geomagnetic storms from the most recent solar maximum. Electron storm time responses are highly dependent on both electron energy and L shell. Tens of keV electrons typically have peak fluxes in the inner belt or near‐Earth plasma sheet and fill the inner magnetosphere during storm main phases. Approximately 100 to ~600 keV electrons are enhanced in up to 87% of cases around L ~3.7, and their peak flux location moves to lower L shells during storm recovery phases. Relativistic electrons (≥~1 MeV) are nearly equally likely to produce enhancement, depletion, and no‐change events in the outer belt. We also show that the L shell of peak flux correlates to storm magnitude only for hundreds of keV electrons. Near L~3.7, ~100 to ~600 keV electrons are enhanced during up to 87% of storm recovery phases Relativistic electrons are split between enhancement, depletion, and no‐change events For hundreds of keV electrons, peak flux L shell after the storm correlates well to storms' SYM‐H minima Nutzungsrecht: © 2015. American Geophysical Union. All Rights Reserved. radiation belts geomagnetic storms electrons Electrons Earth Geophysics Radiation O'Brien, T. P oth Fennell, J. F oth Claudepierre, S. G oth Blake, J. B oth Kilpua, E. K. J oth Hietala, H oth Enthalten in Geophysical research letters Washington, DC : Union, 1974 42(2015), 21, Seite 9176-9184 (DE-627)129095109 (DE-600)7403-2 (DE-576)01443122X 0094-8276 nnns volume:42 year:2015 number:21 pages:9176-9184 http://dx.doi.org/10.1002/2015GL064747 Volltext http://onlinelibrary.wiley.com/doi/10.1002/2015GL064747/abstract http://search.proquest.com/docview/1756229517 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-GEO SSG-OPC-GGO SSG-OPC-GEO GBV_ILN_47 GBV_ILN_62 GBV_ILN_154 GBV_ILN_601 GBV_ILN_2279 38.70 AVZ AR 42 2015 21 9176-9184 |
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10.1002/2015GL064747 doi PQ20160617 (DE-627)OLC1964143772 (DE-599)GBVOLC1964143772 (PRQ)p956-b03942ad5e0b98f6f86f5734b4d5b629552f5d76e7be3ea6087ab5fe7d146dfd0 (KEY)0026932820150000042002109176effectsofgeomagneticstormsonelectronsinearthsradia DE-627 ger DE-627 rakwb eng 550 DNB 38.70 bkl Turner, D. L verfasserin aut The effects of geomagnetic storms on electrons in Earth's radiation belts 2015 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier We use Van Allen Probes data to investigate the responses of tens of keV to 2 MeV electrons throughout a broad range of the radiation belts (2.5 ≤ L ≤ 6.0) during 52 geomagnetic storms from the most recent solar maximum. Electron storm time responses are highly dependent on both electron energy and L shell. Tens of keV electrons typically have peak fluxes in the inner belt or near‐Earth plasma sheet and fill the inner magnetosphere during storm main phases. Approximately 100 to ~600 keV electrons are enhanced in up to 87% of cases around L ~3.7, and their peak flux location moves to lower L shells during storm recovery phases. Relativistic electrons (≥~1 MeV) are nearly equally likely to produce enhancement, depletion, and no‐change events in the outer belt. We also show that the L shell of peak flux correlates to storm magnitude only for hundreds of keV electrons. Near L~3.7, ~100 to ~600 keV electrons are enhanced during up to 87% of storm recovery phases Relativistic electrons are split between enhancement, depletion, and no‐change events For hundreds of keV electrons, peak flux L shell after the storm correlates well to storms' SYM‐H minima Nutzungsrecht: © 2015. American Geophysical Union. All Rights Reserved. radiation belts geomagnetic storms electrons Electrons Earth Geophysics Radiation O'Brien, T. P oth Fennell, J. F oth Claudepierre, S. G oth Blake, J. B oth Kilpua, E. K. J oth Hietala, H oth Enthalten in Geophysical research letters Washington, DC : Union, 1974 42(2015), 21, Seite 9176-9184 (DE-627)129095109 (DE-600)7403-2 (DE-576)01443122X 0094-8276 nnns volume:42 year:2015 number:21 pages:9176-9184 http://dx.doi.org/10.1002/2015GL064747 Volltext http://onlinelibrary.wiley.com/doi/10.1002/2015GL064747/abstract http://search.proquest.com/docview/1756229517 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-GEO SSG-OPC-GGO SSG-OPC-GEO GBV_ILN_47 GBV_ILN_62 GBV_ILN_154 GBV_ILN_601 GBV_ILN_2279 38.70 AVZ AR 42 2015 21 9176-9184 |
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10.1002/2015GL064747 doi PQ20160617 (DE-627)OLC1964143772 (DE-599)GBVOLC1964143772 (PRQ)p956-b03942ad5e0b98f6f86f5734b4d5b629552f5d76e7be3ea6087ab5fe7d146dfd0 (KEY)0026932820150000042002109176effectsofgeomagneticstormsonelectronsinearthsradia DE-627 ger DE-627 rakwb eng 550 DNB 38.70 bkl Turner, D. L verfasserin aut The effects of geomagnetic storms on electrons in Earth's radiation belts 2015 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier We use Van Allen Probes data to investigate the responses of tens of keV to 2 MeV electrons throughout a broad range of the radiation belts (2.5 ≤ L ≤ 6.0) during 52 geomagnetic storms from the most recent solar maximum. Electron storm time responses are highly dependent on both electron energy and L shell. Tens of keV electrons typically have peak fluxes in the inner belt or near‐Earth plasma sheet and fill the inner magnetosphere during storm main phases. Approximately 100 to ~600 keV electrons are enhanced in up to 87% of cases around L ~3.7, and their peak flux location moves to lower L shells during storm recovery phases. Relativistic electrons (≥~1 MeV) are nearly equally likely to produce enhancement, depletion, and no‐change events in the outer belt. We also show that the L shell of peak flux correlates to storm magnitude only for hundreds of keV electrons. Near L~3.7, ~100 to ~600 keV electrons are enhanced during up to 87% of storm recovery phases Relativistic electrons are split between enhancement, depletion, and no‐change events For hundreds of keV electrons, peak flux L shell after the storm correlates well to storms' SYM‐H minima Nutzungsrecht: © 2015. American Geophysical Union. All Rights Reserved. radiation belts geomagnetic storms electrons Electrons Earth Geophysics Radiation O'Brien, T. P oth Fennell, J. F oth Claudepierre, S. G oth Blake, J. B oth Kilpua, E. K. J oth Hietala, H oth Enthalten in Geophysical research letters Washington, DC : Union, 1974 42(2015), 21, Seite 9176-9184 (DE-627)129095109 (DE-600)7403-2 (DE-576)01443122X 0094-8276 nnns volume:42 year:2015 number:21 pages:9176-9184 http://dx.doi.org/10.1002/2015GL064747 Volltext http://onlinelibrary.wiley.com/doi/10.1002/2015GL064747/abstract http://search.proquest.com/docview/1756229517 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-GEO SSG-OPC-GGO SSG-OPC-GEO GBV_ILN_47 GBV_ILN_62 GBV_ILN_154 GBV_ILN_601 GBV_ILN_2279 38.70 AVZ AR 42 2015 21 9176-9184 |
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10.1002/2015GL064747 doi PQ20160617 (DE-627)OLC1964143772 (DE-599)GBVOLC1964143772 (PRQ)p956-b03942ad5e0b98f6f86f5734b4d5b629552f5d76e7be3ea6087ab5fe7d146dfd0 (KEY)0026932820150000042002109176effectsofgeomagneticstormsonelectronsinearthsradia DE-627 ger DE-627 rakwb eng 550 DNB 38.70 bkl Turner, D. L verfasserin aut The effects of geomagnetic storms on electrons in Earth's radiation belts 2015 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier We use Van Allen Probes data to investigate the responses of tens of keV to 2 MeV electrons throughout a broad range of the radiation belts (2.5 ≤ L ≤ 6.0) during 52 geomagnetic storms from the most recent solar maximum. Electron storm time responses are highly dependent on both electron energy and L shell. Tens of keV electrons typically have peak fluxes in the inner belt or near‐Earth plasma sheet and fill the inner magnetosphere during storm main phases. Approximately 100 to ~600 keV electrons are enhanced in up to 87% of cases around L ~3.7, and their peak flux location moves to lower L shells during storm recovery phases. Relativistic electrons (≥~1 MeV) are nearly equally likely to produce enhancement, depletion, and no‐change events in the outer belt. We also show that the L shell of peak flux correlates to storm magnitude only for hundreds of keV electrons. Near L~3.7, ~100 to ~600 keV electrons are enhanced during up to 87% of storm recovery phases Relativistic electrons are split between enhancement, depletion, and no‐change events For hundreds of keV electrons, peak flux L shell after the storm correlates well to storms' SYM‐H minima Nutzungsrecht: © 2015. American Geophysical Union. All Rights Reserved. radiation belts geomagnetic storms electrons Electrons Earth Geophysics Radiation O'Brien, T. P oth Fennell, J. F oth Claudepierre, S. G oth Blake, J. B oth Kilpua, E. K. J oth Hietala, H oth Enthalten in Geophysical research letters Washington, DC : Union, 1974 42(2015), 21, Seite 9176-9184 (DE-627)129095109 (DE-600)7403-2 (DE-576)01443122X 0094-8276 nnns volume:42 year:2015 number:21 pages:9176-9184 http://dx.doi.org/10.1002/2015GL064747 Volltext http://onlinelibrary.wiley.com/doi/10.1002/2015GL064747/abstract http://search.proquest.com/docview/1756229517 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-GEO SSG-OPC-GGO SSG-OPC-GEO GBV_ILN_47 GBV_ILN_62 GBV_ILN_154 GBV_ILN_601 GBV_ILN_2279 38.70 AVZ AR 42 2015 21 9176-9184 |
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10.1002/2015GL064747 doi PQ20160617 (DE-627)OLC1964143772 (DE-599)GBVOLC1964143772 (PRQ)p956-b03942ad5e0b98f6f86f5734b4d5b629552f5d76e7be3ea6087ab5fe7d146dfd0 (KEY)0026932820150000042002109176effectsofgeomagneticstormsonelectronsinearthsradia DE-627 ger DE-627 rakwb eng 550 DNB 38.70 bkl Turner, D. L verfasserin aut The effects of geomagnetic storms on electrons in Earth's radiation belts 2015 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier We use Van Allen Probes data to investigate the responses of tens of keV to 2 MeV electrons throughout a broad range of the radiation belts (2.5 ≤ L ≤ 6.0) during 52 geomagnetic storms from the most recent solar maximum. Electron storm time responses are highly dependent on both electron energy and L shell. Tens of keV electrons typically have peak fluxes in the inner belt or near‐Earth plasma sheet and fill the inner magnetosphere during storm main phases. Approximately 100 to ~600 keV electrons are enhanced in up to 87% of cases around L ~3.7, and their peak flux location moves to lower L shells during storm recovery phases. Relativistic electrons (≥~1 MeV) are nearly equally likely to produce enhancement, depletion, and no‐change events in the outer belt. We also show that the L shell of peak flux correlates to storm magnitude only for hundreds of keV electrons. Near L~3.7, ~100 to ~600 keV electrons are enhanced during up to 87% of storm recovery phases Relativistic electrons are split between enhancement, depletion, and no‐change events For hundreds of keV electrons, peak flux L shell after the storm correlates well to storms' SYM‐H minima Nutzungsrecht: © 2015. American Geophysical Union. All Rights Reserved. radiation belts geomagnetic storms electrons Electrons Earth Geophysics Radiation O'Brien, T. P oth Fennell, J. F oth Claudepierre, S. G oth Blake, J. B oth Kilpua, E. K. J oth Hietala, H oth Enthalten in Geophysical research letters Washington, DC : Union, 1974 42(2015), 21, Seite 9176-9184 (DE-627)129095109 (DE-600)7403-2 (DE-576)01443122X 0094-8276 nnns volume:42 year:2015 number:21 pages:9176-9184 http://dx.doi.org/10.1002/2015GL064747 Volltext http://onlinelibrary.wiley.com/doi/10.1002/2015GL064747/abstract http://search.proquest.com/docview/1756229517 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-GEO SSG-OPC-GGO SSG-OPC-GEO GBV_ILN_47 GBV_ILN_62 GBV_ILN_154 GBV_ILN_601 GBV_ILN_2279 38.70 AVZ AR 42 2015 21 9176-9184 |
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The effects of geomagnetic storms on electrons in Earth's radiation belts |
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The effects of geomagnetic storms on electrons in Earth's radiation belts |
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effects of geomagnetic storms on electrons in earth's radiation belts |
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The effects of geomagnetic storms on electrons in Earth's radiation belts |
| abstract |
We use Van Allen Probes data to investigate the responses of tens of keV to 2 MeV electrons throughout a broad range of the radiation belts (2.5 ≤ L ≤ 6.0) during 52 geomagnetic storms from the most recent solar maximum. Electron storm time responses are highly dependent on both electron energy and L shell. Tens of keV electrons typically have peak fluxes in the inner belt or near‐Earth plasma sheet and fill the inner magnetosphere during storm main phases. Approximately 100 to ~600 keV electrons are enhanced in up to 87% of cases around L ~3.7, and their peak flux location moves to lower L shells during storm recovery phases. Relativistic electrons (≥~1 MeV) are nearly equally likely to produce enhancement, depletion, and no‐change events in the outer belt. We also show that the L shell of peak flux correlates to storm magnitude only for hundreds of keV electrons. Near L~3.7, ~100 to ~600 keV electrons are enhanced during up to 87% of storm recovery phases Relativistic electrons are split between enhancement, depletion, and no‐change events For hundreds of keV electrons, peak flux L shell after the storm correlates well to storms' SYM‐H minima |
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We use Van Allen Probes data to investigate the responses of tens of keV to 2 MeV electrons throughout a broad range of the radiation belts (2.5 ≤ L ≤ 6.0) during 52 geomagnetic storms from the most recent solar maximum. Electron storm time responses are highly dependent on both electron energy and L shell. Tens of keV electrons typically have peak fluxes in the inner belt or near‐Earth plasma sheet and fill the inner magnetosphere during storm main phases. Approximately 100 to ~600 keV electrons are enhanced in up to 87% of cases around L ~3.7, and their peak flux location moves to lower L shells during storm recovery phases. Relativistic electrons (≥~1 MeV) are nearly equally likely to produce enhancement, depletion, and no‐change events in the outer belt. We also show that the L shell of peak flux correlates to storm magnitude only for hundreds of keV electrons. Near L~3.7, ~100 to ~600 keV electrons are enhanced during up to 87% of storm recovery phases Relativistic electrons are split between enhancement, depletion, and no‐change events For hundreds of keV electrons, peak flux L shell after the storm correlates well to storms' SYM‐H minima |
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We use Van Allen Probes data to investigate the responses of tens of keV to 2 MeV electrons throughout a broad range of the radiation belts (2.5 ≤ L ≤ 6.0) during 52 geomagnetic storms from the most recent solar maximum. Electron storm time responses are highly dependent on both electron energy and L shell. Tens of keV electrons typically have peak fluxes in the inner belt or near‐Earth plasma sheet and fill the inner magnetosphere during storm main phases. Approximately 100 to ~600 keV electrons are enhanced in up to 87% of cases around L ~3.7, and their peak flux location moves to lower L shells during storm recovery phases. Relativistic electrons (≥~1 MeV) are nearly equally likely to produce enhancement, depletion, and no‐change events in the outer belt. We also show that the L shell of peak flux correlates to storm magnitude only for hundreds of keV electrons. Near L~3.7, ~100 to ~600 keV electrons are enhanced during up to 87% of storm recovery phases Relativistic electrons are split between enhancement, depletion, and no‐change events For hundreds of keV electrons, peak flux L shell after the storm correlates well to storms' SYM‐H minima |
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The effects of geomagnetic storms on electrons in Earth's radiation belts |
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http://dx.doi.org/10.1002/2015GL064747 http://onlinelibrary.wiley.com/doi/10.1002/2015GL064747/abstract http://search.proquest.com/docview/1756229517 |
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O'Brien, T. P Fennell, J. F Claudepierre, S. G Blake, J. B Kilpua, E. K. J Hietala, H |
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