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Lifetime of energetic electrons due to their interactions with chorus waves

Authors
/persons/resource/dedong

Wang,  D.
2.7 Space Physics and Space Weather, 2.0 Geophysics, Departments, GFZ Publication Database, Deutsches GeoForschungsZentrum;
IUGG 2023, General Assemblies, 1 General, International Union of Geodesy and Geophysics (IUGG), External Organizations;

/persons/resource/yshprits

SHPRITS,  YURI
2.7 Space Physics and Space Weather, 2.0 Geophysics, Departments, GFZ Publication Database, Deutsches GeoForschungsZentrum;
IUGG 2023, General Assemblies, 1 General, International Union of Geodesy and Geophysics (IUGG), External Organizations;

/persons/resource/bhaas

Haas,  Bernhard
2.7 Space Physics and Space Weather, 2.0 Geophysics, Departments, GFZ Publication Database, Deutsches GeoForschungsZentrum;
IUGG 2023, General Assemblies, 1 General, International Union of Geodesy and Geophysics (IUGG), External Organizations;

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Citation

Wang, D., SHPRITS, Y., Haas, B. (2023): Lifetime of energetic electrons due to their interactions with chorus waves, XXVIII General Assembly of the International Union of Geodesy and Geophysics (IUGG) (Berlin 2023).
https://doi.org/10.57757/IUGG23-4368


Cite as: https://gfzpublic.gfz-potsdam.de/pubman/item/item_5021799
Abstract
Energetic electrons in the Earth's magnetosphere can be dangerous to satellites. Chorus waves can cause the loss of energetic electrons in this area via pitch-angle scattering. To quantify the effect of chorus waves on energetic electrons, we calculate the bounce-averaged quasi-linear diffusion coefficients. In this study, using these diffusion coefficients, we calculated the lifetime of the electrons with an energy range from 1 keV to 2 MeV using two different methods. We parameterize the electron lifetime as a function of L-shell and electron kinetic energy in each MLT and geomagnetic activity (Kp). The parameterized electron lifetimes show a strong functional dependence on L-shell and electron energy. This new model of electron lifetime is more advanced than previous models. In particular, the current model fills the gap that previous models have on the dusk side of the Earth's magnetosphere. This improvement is critical for radiation belt and ring current modeling studies.