Properties of relativistic electron precipitation: a comparative analysis of wave-induced and field line curvature scattering processes
We analyze the properties of relativistic (>700 keV) electron precipitation (REP) events measured by the low-Earth-orbit (LEO) POES/MetOp constellation of spacecraft from 2012 through 2023. Leveraging the different profiles of REP observed at LEO, we associate each event with its possible dri...
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Frontiers Media S.A.
2024-11-01
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| Series: | Frontiers in Astronomy and Space Sciences |
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| Online Access: | https://www.frontiersin.org/articles/10.3389/fspas.2024.1495008/full |
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| author | Luisa Capannolo Andrew Staff Wen Li Katharine Duderstadt Nithin Sivadas Nithin Sivadas Joshua Pettit Joshua Pettit Sadie Elliot Murong Qin Xiao-Chen Shen Qianli Ma Qianli Ma |
| author_facet | Luisa Capannolo Andrew Staff Wen Li Katharine Duderstadt Nithin Sivadas Nithin Sivadas Joshua Pettit Joshua Pettit Sadie Elliot Murong Qin Xiao-Chen Shen Qianli Ma Qianli Ma |
| author_sort | Luisa Capannolo |
| collection | DOAJ |
| description | We analyze the properties of relativistic (>700 keV) electron precipitation (REP) events measured by the low-Earth-orbit (LEO) POES/MetOp constellation of spacecraft from 2012 through 2023. Leveraging the different profiles of REP observed at LEO, we associate each event with its possible driver: waves or field line curvature scattering (FLCS). While waves typically precipitate electrons in a localized radial region within the outer radiation belt, FLCS drives energy-dependent precipitation at the edge of the belt. Wave-driven REP is detected at any MLT sector and L shell, with FLCS-driven REP occurring only over the nightside–a region where field line stretching is frequent. Wave-driven REP is broader in radial extent on the dayside and accompanied by proton precipitation over 03–23 MLT, either isolated or without a clear energy-dependent pattern, possibly implying that electromagnetic ion cyclotron (EMIC) waves are the primary driver. Across midnight, both wave-driven and FLCS-driven REP occur poleward of the proton isotropic boundary. On average, waves precipitate a higher flux of >700 keV electrons than FLCS. Both contribute to energy deposition into the atmosphere, estimated of a few MW. REP is more associated with substorm activity than storms, with FLCS-driven REP and wave-driven REP at low L shells occurring most often during strong activity (SML* < −600 nT). A preliminary analysis of the Solar Wind (SW) properties before the observed REP indicates a more sustained (∼5 h) dayside reconnection for FLCS-driven REP than for wave-driven REP (∼3 h). The magnetosphere appears more compressed during wave-driven REP, while FLCS-driven REP is associated with a faster SW of lower density. These findings are useful not only to quantify the contribution of >700 keV precipitation to the atmosphere but also to shed light on the typical properties of wave-driven vs FLCS-driven precipitation which can be assimilated into physics-based and/or predictive radiation belt models. In addition, the dataset of ∼9,400 REP events is made available to the community to enable future work. |
| format | Article |
| id | doaj-art-c8eb13b0649e4abea8fcc4afc8597e08 |
| institution | OA Journals |
| issn | 2296-987X |
| language | English |
| publishDate | 2024-11-01 |
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| spelling | doaj-art-c8eb13b0649e4abea8fcc4afc8597e082025-08-20T02:13:07ZengFrontiers Media S.A.Frontiers in Astronomy and Space Sciences2296-987X2024-11-011110.3389/fspas.2024.14950081495008Properties of relativistic electron precipitation: a comparative analysis of wave-induced and field line curvature scattering processesLuisa Capannolo0Andrew Staff1Wen Li2Katharine Duderstadt3Nithin Sivadas4Nithin Sivadas5Joshua Pettit6Joshua Pettit7Sadie Elliot8Murong Qin9Xiao-Chen Shen10Qianli Ma11Qianli Ma12Center for Space Physics, Boston University, Boston, MA, United StatesCenter for Space Physics, Boston University, Boston, MA, United StatesCenter for Space Physics, Boston University, Boston, MA, United StatesEarth Systems Research Center, University of New Hampshire, Durham, NH, United StatesSpace Weather Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD, United StatesDepartment of Physics, The Catholic University of America, Washington DC, MD, United StatesSpace Weather Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD, United StatesCollege of Science, George Mason University, Fairfax, VA, United StatesSchool of Physics and Astronomy, College of Science and Engineering, University of Minnesota, Minneapolis, MN, United StatesCenter for Space Physics, Boston University, Boston, MA, United StatesCenter for Space Physics, Boston University, Boston, MA, United StatesCenter for Space Physics, Boston University, Boston, MA, United StatesDepartment of Atmospheric and Oceanic Sciences, University of California Los Angeles, Los Angeles, CA, United StatesWe analyze the properties of relativistic (>700 keV) electron precipitation (REP) events measured by the low-Earth-orbit (LEO) POES/MetOp constellation of spacecraft from 2012 through 2023. Leveraging the different profiles of REP observed at LEO, we associate each event with its possible driver: waves or field line curvature scattering (FLCS). While waves typically precipitate electrons in a localized radial region within the outer radiation belt, FLCS drives energy-dependent precipitation at the edge of the belt. Wave-driven REP is detected at any MLT sector and L shell, with FLCS-driven REP occurring only over the nightside–a region where field line stretching is frequent. Wave-driven REP is broader in radial extent on the dayside and accompanied by proton precipitation over 03–23 MLT, either isolated or without a clear energy-dependent pattern, possibly implying that electromagnetic ion cyclotron (EMIC) waves are the primary driver. Across midnight, both wave-driven and FLCS-driven REP occur poleward of the proton isotropic boundary. On average, waves precipitate a higher flux of >700 keV electrons than FLCS. Both contribute to energy deposition into the atmosphere, estimated of a few MW. REP is more associated with substorm activity than storms, with FLCS-driven REP and wave-driven REP at low L shells occurring most often during strong activity (SML* < −600 nT). A preliminary analysis of the Solar Wind (SW) properties before the observed REP indicates a more sustained (∼5 h) dayside reconnection for FLCS-driven REP than for wave-driven REP (∼3 h). The magnetosphere appears more compressed during wave-driven REP, while FLCS-driven REP is associated with a faster SW of lower density. These findings are useful not only to quantify the contribution of >700 keV precipitation to the atmosphere but also to shed light on the typical properties of wave-driven vs FLCS-driven precipitation which can be assimilated into physics-based and/or predictive radiation belt models. In addition, the dataset of ∼9,400 REP events is made available to the community to enable future work.https://www.frontiersin.org/articles/10.3389/fspas.2024.1495008/fullradiation beltselectron precipitationfield line curvature scatteringwave-particle interactionsatmospheric energy inputprecipitating electron flux |
| spellingShingle | Luisa Capannolo Andrew Staff Wen Li Katharine Duderstadt Nithin Sivadas Nithin Sivadas Joshua Pettit Joshua Pettit Sadie Elliot Murong Qin Xiao-Chen Shen Qianli Ma Qianli Ma Properties of relativistic electron precipitation: a comparative analysis of wave-induced and field line curvature scattering processes Frontiers in Astronomy and Space Sciences radiation belts electron precipitation field line curvature scattering wave-particle interactions atmospheric energy input precipitating electron flux |
| title | Properties of relativistic electron precipitation: a comparative analysis of wave-induced and field line curvature scattering processes |
| title_full | Properties of relativistic electron precipitation: a comparative analysis of wave-induced and field line curvature scattering processes |
| title_fullStr | Properties of relativistic electron precipitation: a comparative analysis of wave-induced and field line curvature scattering processes |
| title_full_unstemmed | Properties of relativistic electron precipitation: a comparative analysis of wave-induced and field line curvature scattering processes |
| title_short | Properties of relativistic electron precipitation: a comparative analysis of wave-induced and field line curvature scattering processes |
| title_sort | properties of relativistic electron precipitation a comparative analysis of wave induced and field line curvature scattering processes |
| topic | radiation belts electron precipitation field line curvature scattering wave-particle interactions atmospheric energy input precipitating electron flux |
| url | https://www.frontiersin.org/articles/10.3389/fspas.2024.1495008/full |
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