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Modeling the Dynamics of Radiation Belt Electrons With Source and Loss Driven by the Solar Wind


Metadata FieldValueLanguage
dc.creatorXiang, Zheng
dc.creatorLi, Xinlin
dc.creatorKapali, Sudha
dc.creatorGannon, Jennifer
dc.creatorNi, Binbin
dc.creatorZhao, Hong
dc.creatorZhang, Kun
dc.creatorKhoo, Leng Ying
dc.date.accessioned2022-11-16T20:58:56Z
dc.date.available2022-11-16T20:58:56Z
dc.date.created2021
dc.identifier10.1029/2020JA028988en_US
dc.identifier.urihttps://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2020JA028988en_US
dc.identifier.urihttps://aurora.auburn.edu/handle/11200/50462
dc.identifier.urihttp://dx.doi.org/10.35099/aurora-530
dc.description.abstractA radial diffusion model directly driven by the solar wind is developed to reproduce MeV electron variations between L = 2-12 (L is L* in this study) from October 2012 to April 2015. The radial diffusion coefficient, internal source rate, quick loss due to EMIC waves, and slow loss due to hiss waves are all expressed in terms of the solar wind speed, dynamic pressure, and interplanetary magnetic field (IMF). The model achieves a prediction efficiency (PE) of 0.45 at L = 5 and 0.51 at L = 4 after converting the electron phase space densities to differential fluxes and comparing with Van Allen Probes measurements of 2 and 3 MeV electrons at L = 5 and L = 4, respectively. Machine learning techniques are used to tune parameters to get higher PE. By tuning parameters for every 60-day period, the model obtains PE values of 0.58 and 0.82 at L = 5 and L = 4, respectively. Inspired by these results, we divide the solar wind activity into three categories based on the condition of solar wind speed, IMF Bz, and dynamic pressure, and then tune these three sets of parameters to obtain the highest PE. This experiment confirms that the solar wind speed has the greatest influence on the electron flux variations, particularly at higher L, while the dynamic pressure has more influence at lower L. Also, the PE at L = 4 is mostly higher than those at L = 5, suggesting that the electron loss due to the magnetopause shadowing combined with the outward radial diffusion is not well captured in the model.en_US
dc.formatPDFen_US
dc.publisherAmerican Geophysical Unionen_US
dc.relation.ispartofJOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICSen_US
dc.relation.ispartofseries2169-9380en_US
dc.rights©American Geophysical Union 2021. This is this the version of record co-published by the American Geophysical Union and John Wiley & Sons, Inc. It is made available under the CC-BY-NC-ND 4.0 license. Item should be cited as: Xiang, Z., Li, X., Kapali, S., Gannon, J., Ni, B., Zhao, H., ... & Khoo, L. Y. (2021). Modeling the dynamics of radiation belt electrons with source and loss driven by the solar wind. Journal of Geophysical Research: Space Physics, 126(6), e2020JA028988.en_US
dc.titleModeling the Dynamics of Radiation Belt Electrons With Source and Loss Driven by the Solar Winden_US
dc.typeTexten_US
dc.type.genreJournal Article, Academic Journalen_US
dc.citation.volume126en_US
dc.citation.issue6en_US
dc.description.statusPublisheden_US
dc.description.peerreviewYesen_US
dc.creator.orcid0000-0003-0393-9833en_US
dc.creator.orcid0000-0001-8292-7691en_US
dc.creator.orcid0000-0002-4899-7917en_US
dc.creator.orcid0000-0003-0412-1064en_US
dc.creator.orcid0000-0002-1683-3192en_US

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