Effects of the solar wind on magnetospheric dynamics: Energetic electrons at the synchronous orbit

By G. Paulikas, J. Bernard Blake. 2013

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View Paper: https://www.semanticscholar.org/paper/3224d68fb552bb5c7f6ed1c7c87b1db6ae3de7b2

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In Astronomy and Astrophysics

Citations in the corpus

Discovery of very large amplitude whistler‐mode waves in Earth's radiation belts (2008, result): “Thus, the STEREO observations are consistent with studies correlating enhanced fluxes with high speed streams [Paulikas and Blake, 1979].”
Ring current ions and radiation belt electrons during geomagnetic storms driven by coronal mass ejections and corotating interaction regions (2005, background): “[17] A good correlation between the outer belt enhancement and the solar wind speed has been shown [e.g., Paulikas and Blake, 1979], and the previous studies considered the solar wind speed as a primary parameter for the evolution of the outer belt [e.g., Mathie and Mann, 2001].”
On the relationship between relativistic electron flux and solar wind velocity: Paulikas and Blake revisited (2010, background): “(top) Reproduced plots from Paulikas and Blake [1979] showing 36 h, 27 day, and 6 month averages for integral energies >1.”
Energization of relativistic electrons in the presence of ULF power and mev microbursts: Evidence for dual ULF and VLF acceleration (2003, background): “…of magnetic activity or high solar wind velocity and the peak in the radiation belt fluxes for fluxes of 3 MeV electrons at geosynchronous orbit [Paulikas and Blake, 1979; Baker et al., 1990], or 1–2 days for lowaltitude fluxes of >400 keV electrons over a range of L values [Baker et al., 1994].”
Electron losses from the radiation belts caused by EMIC waves (2014, background): “In contrast to the inner belt the electron fluxes in the outer belt are highly variable [Paulikas and Blake, 1979; Baker et al., 1986].”
Global morphology and spectral properties of EMIC waves derived from CRRES observations (2014, background): “However, the outer radiation belt, which extends from 3 to 7 RE , is highly variable [Paulikas and Blake, 1979; Baker et al., 1986].”
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): “…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; Miyoshi and Kataoka, 2005].”
Space Weather Effects in the Earth’s Radiation Belts (2018, background): “Paulikas and Blake (1979), for example, analyzed energetic electron data from ATS-1, ATS-5 and ATS-6 spacecraft and found a pronounced positive correlation between the electron fluxes and solar wind speed.”