Ring current ions and radiation belt electrons during geomagnetic storms driven by coronal mass ejections and corotating interaction regions

By Yoshizumi Miyoshi, R. Kataoka. 2005

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Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/3d8187b292fe9209dff403234bfec88f793c2736

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Timescales for radiation belt electron acceleration and loss due to resonant wave-particle interactions: 1. Theory (2007, background): “…radiation belt (3 < L < 7) is highly variable, particularly during magnetic storms or other geomagnetically disturbed periods [e.g., Paulikas and Blake, 1979; Baker et al., 1986, 1994, 1997; Li et al., 1997; Reeves et al., 1998; Obara et al., 2000;Miyoshi et al., 2003; Miyoshi and Kataoka, 2005].”
Use of POES SEM-2 observations to examine radiation belt dynamics and energetic electron precipitation into the atmosphere (2010, background): “It has been suggested that there are more long‐lasting radiation belt electron flux enhancements in HSSWS‐driven storms compared to ICME‐driven storms [ Miyoshi and Kataoka, 2005 ], that the flux of higher‐energy particles peak later in time, and that many magnetospheric electromagnetic wave process”
Geoeffectiveness of halo coronal mass ejections (2007, background): “About 10% of strong storms are caused by CIRs, but the Dst values are generally not too far below 100 nT [see, e.g., Sheeley et al., 1976; Miyoshi and Kataoka, 2005; Richardson et al., 2006].”
Relativistic electron precipitation by EMIC waves from self‐consistent global simulations (2008, background): “Even for modest geomagnetic storms, radiation belt electron fluxes can be rapidly enhanced within the Earth’s inner magnetosphere [e.g., Miyoshi and Kataoka, 2005; Baker and Kanekal, 2007].”
High‐speed solar wind with southward interplanetary magnetic field causes relativistic electron flux enhancement of the outer radiation belt via enhanced condition of whistler waves (2013, background): “[17] The relativistic electron flux of the outer radiation belt tends to increase largely during the recovery phase of CIR-driven storms rather than during coronal mass ejection (CME)-driven storms [Miyoshi and Kataoka, 2005; Kataoka and Miyoshi, 2006].”
Relativistic electron loss timescales in the slot region (2009, background): “In contrast, the outer radiation belt, which usually lies between 3 Miyoshi and Kataoka, 2005 ].”
Geospace exploration project ERG (2018, background): “The flux then recovers and often significantly increases during the recovery phase of storms (e.g., Nagai 1988; Miyoshi and Kataoka 2005).”
Precipitation of radiation belt electrons by EMIC waves, observed from ground and space (2008, background): “[2] Populations of relativistic electrons in the radiation belts vary greatly with geomagnetic disturbance [e.g., Reeves et al., 2003; Miyoshi and Kataoka, 2005 ] and they are a major source of damage to space vehicles [e.g., Baker et al., 1987].”
Major geomagnetic storms (Dst<=-100~nT) generated by corotating interaction regions in 1996--2004 (2006, background): “CIRs are known, for example, to have a greater influence on the strength of the outer radiation belts than CME-driven storms [e.g., Paulikas and Blake, 1976; Lam, 2004; Miyoshi and Kataoka, 2005 ].”
The Interaction of Successive Coronal Mass Ejections: A Review (2016, background): “…et al., 1991; Webb et al., 2000; Zhang et al., 2007), and they are also associated with many of the strongest substorms (Kamide et al., 1998; Tsurutani et al., 2015), changes in Earth radiation belts (Miyoshi and Kataoka, 2005) and geomagnetically-induced currents (GICs) (Huttunen et al., 2008).”
Three‐dimensional electron radiation belt simulations using the BAS Radiation Belt Model with new diffusion models for chorus, plasmaspheric hiss, and lightning‐generated whistlers (2014, background): “The electron population in the inner belt is relatively stable, but the population in the outer belt is highly variable, especially during geomagnetic storms which are ultimately driven by the solar wind [Paulikas and Blake, 1979; Baker et al., 1986, 1994, 1997; Li et al., 1997; Reeves et al., 1998;”
Relativistic turning acceleration of resonant electrons by coherent whistler mode waves in a dipole magnetic field (2007, background): “[2] Over the course of a geomagnetic storm, the flux of relativistic (>1 MeV) electrons in the outer radiation belt (3 Miyoshi and Kataoka [2005] .”