A Framework for Understanding and Quantifying the Loss and Acceleration of Relativistic Electrons in the Outer Radiation Belt During Geomagnetic Storms
Abstract We present detailed analysis of the global relativistic electron dynamics as measured by total radiation belt content (RBC) during coronal mass ejection (CME) and corotating interaction region (CIR)‐driven geomagnetic storms. Recent work has demonstrated that the response of the outer radia...
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Wiley
2020-05-01
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| Series: | Space Weather |
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| Online Access: | https://doi.org/10.1029/2020SW002477 |
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| author | Kyle R. Murphy Ian R. Mann David G. Sibeck I. Jonathan Rae C.E.J. Watt Louis G. Ozeke Shri G. Kanekal Daniel N. Baker |
| author_facet | Kyle R. Murphy Ian R. Mann David G. Sibeck I. Jonathan Rae C.E.J. Watt Louis G. Ozeke Shri G. Kanekal Daniel N. Baker |
| author_sort | Kyle R. Murphy |
| collection | DOAJ |
| description | Abstract We present detailed analysis of the global relativistic electron dynamics as measured by total radiation belt content (RBC) during coronal mass ejection (CME) and corotating interaction region (CIR)‐driven geomagnetic storms. Recent work has demonstrated that the response of the outer radiation belt is consistent and repeatable during geomagnetic storms. Here we build on this work to show that radiation belt dynamics can be divided into two sequential phases, which have different solar wind dependencies and which when analyzed separately reveal that the radiation belt responds more predictably than if the overall storm response is analyzed as a whole. In terms of RBC, in every storm we analyzed, a phase dominated by loss is followed by a phase dominated by acceleration. Analysis of the RBC during each of these phases demonstrates that they both respond coherently to solar wind and magnetospheric driving. However, the response is independent of whether the storm response is associated with either a CME or CIR. Our analysis shows that during the initial phase, radiation belt loss is organized by the location of the magnetopause and the strength of Dst and ultralow frequency wave power. During the second phase, radiation belt enhancements are well organized by the amplitude of ultralow frequency waves, the auroral electroject index, and solar wind energy input. Overall, our results demonstrate that storm time dynamics of the RBC is repeatable and well characterized by solar wind and geomagnetic driving, albeit with different dependencies during the two phases of a storm. |
| format | Article |
| id | doaj-art-e82c5183615f41938775066587a59c78 |
| institution | Kabale University |
| issn | 1542-7390 |
| language | English |
| publishDate | 2020-05-01 |
| publisher | Wiley |
| record_format | Article |
| series | Space Weather |
| spelling | doaj-art-e82c5183615f41938775066587a59c782025-01-14T16:27:36ZengWileySpace Weather1542-73902020-05-01185n/an/a10.1029/2020SW002477A Framework for Understanding and Quantifying the Loss and Acceleration of Relativistic Electrons in the Outer Radiation Belt During Geomagnetic StormsKyle R. Murphy0Ian R. Mann1David G. Sibeck2I. Jonathan Rae3C.E.J. Watt4Louis G. Ozeke5Shri G. Kanekal6Daniel N. Baker7Department of Astronomy University of Maryland College Park MD USANASA Goddard Space Flight Centre Code 674 Greenbelt MD USANASA Goddard Space Flight Centre Code 674 Greenbelt MD USADepartment of Space and Climate Physics, Mullard Space Science Laboratory University College London London UKDepartment of Meteorology University of Reading Reading UKDepartment of Physics University of Alberta Edmonton Alberta CanadaNASA Goddard Space Flight Centre Code 674 Greenbelt MD USALaboratory for Atmospheric and Space Physics University of Colorado Boulder Boulder CO USAAbstract We present detailed analysis of the global relativistic electron dynamics as measured by total radiation belt content (RBC) during coronal mass ejection (CME) and corotating interaction region (CIR)‐driven geomagnetic storms. Recent work has demonstrated that the response of the outer radiation belt is consistent and repeatable during geomagnetic storms. Here we build on this work to show that radiation belt dynamics can be divided into two sequential phases, which have different solar wind dependencies and which when analyzed separately reveal that the radiation belt responds more predictably than if the overall storm response is analyzed as a whole. In terms of RBC, in every storm we analyzed, a phase dominated by loss is followed by a phase dominated by acceleration. Analysis of the RBC during each of these phases demonstrates that they both respond coherently to solar wind and magnetospheric driving. However, the response is independent of whether the storm response is associated with either a CME or CIR. Our analysis shows that during the initial phase, radiation belt loss is organized by the location of the magnetopause and the strength of Dst and ultralow frequency wave power. During the second phase, radiation belt enhancements are well organized by the amplitude of ultralow frequency waves, the auroral electroject index, and solar wind energy input. Overall, our results demonstrate that storm time dynamics of the RBC is repeatable and well characterized by solar wind and geomagnetic driving, albeit with different dependencies during the two phases of a storm.https://doi.org/10.1029/2020SW002477radiation belt dynamicsgeomagnetic stormsradiation belt lossradiation belt enhancementloss driversenhancement drivers |
| spellingShingle | Kyle R. Murphy Ian R. Mann David G. Sibeck I. Jonathan Rae C.E.J. Watt Louis G. Ozeke Shri G. Kanekal Daniel N. Baker A Framework for Understanding and Quantifying the Loss and Acceleration of Relativistic Electrons in the Outer Radiation Belt During Geomagnetic Storms Space Weather radiation belt dynamics geomagnetic storms radiation belt loss radiation belt enhancement loss drivers enhancement drivers |
| title | A Framework for Understanding and Quantifying the Loss and Acceleration of Relativistic Electrons in the Outer Radiation Belt During Geomagnetic Storms |
| title_full | A Framework for Understanding and Quantifying the Loss and Acceleration of Relativistic Electrons in the Outer Radiation Belt During Geomagnetic Storms |
| title_fullStr | A Framework for Understanding and Quantifying the Loss and Acceleration of Relativistic Electrons in the Outer Radiation Belt During Geomagnetic Storms |
| title_full_unstemmed | A Framework for Understanding and Quantifying the Loss and Acceleration of Relativistic Electrons in the Outer Radiation Belt During Geomagnetic Storms |
| title_short | A Framework for Understanding and Quantifying the Loss and Acceleration of Relativistic Electrons in the Outer Radiation Belt During Geomagnetic Storms |
| title_sort | framework for understanding and quantifying the loss and acceleration of relativistic electrons in the outer radiation belt during geomagnetic storms |
| topic | radiation belt dynamics geomagnetic storms radiation belt loss radiation belt enhancement loss drivers enhancement drivers |
| url | https://doi.org/10.1029/2020SW002477 |
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