Unraveling the drivers of the storm time radiation belt response
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- E. K. J. Kilpua
- Department of Physics University of Helsinki Helsinki Finland
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- H. Hietala
- The Blackett Laboratory Imperial College London London UK
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- D. L. Turner
- The Aerospace Corporation Los Angeles California USA
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- H. E. J. Koskinen
- Department of Physics University of Helsinki Helsinki Finland
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- T. I. Pulkkinen
- Department of Radio Science and Engineering Aalto University Aalto Finland
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- J. V. Rodriguez
- Cooperative Institute for Research in Environmental Sciences University of Colorado Boulder Boulder Colorado USA
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- G. D. Reeves
- Los Alamos National Laboratory Los Alamos New Mexico USA
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- S. G. Claudepierre
- The Aerospace Corporation Los Angeles California USA
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- H. E. Spence
- Institute for the Study of Earth, Oceans, and Space University of New Hampshire Durham New Hampshire USA
書誌事項
- 公開日
- 2015-05-04
- 権利情報
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- http://onlinelibrary.wiley.com/termsAndConditions#vor
- DOI
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- 10.1002/2015gl063542
- 公開者
- American Geophysical Union (AGU)
この論文をさがす
説明
<jats:title>Abstract</jats:title><jats:p>We present a new framework to study the time evolution and dynamics of the outer Van Allen belt electron fluxes. The framework is entirely based on the large‐scale solar wind storm drivers and their substructures. The Van Allen Probe observations, revealing the electron flux behavior throughout the outer belt, are combined with continuous, long‐term (over 1.5 solar cycles) geosynchronous orbit data set from GOES and solar wind measurements A superposed epoch analysis, where we normalize the timescales for each substructure (sheath, ejecta, and interface region) allows us to avoid smearing effects and to distinguish the electron flux evolution during various driver structures. We show that the radiation belt response is not random: The electron flux variations are determined by the combined effect of the structured solar wind driver and prestorm electron flux levels. In particular, we find that loss mechanisms dominate during stream interface regions, coronal mass ejection (CME) ejecta, and sheaths while enhancements occur during fast streams trailing the stream interface or the CME.</jats:p>
収録刊行物
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- Geophysical Research Letters
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Geophysical Research Letters 42 (9), 3076-3084, 2015-05-04
American Geophysical Union (AGU)
