Impact of Solar Wind on the Earth Magnetosphere: Recent Progress in the Modeling of Ring Current and Radiation Belts

Recovery phase of magnetic storms induced by different interplanetary drivers

“…Therefore interplanetary drivers of magnetic storms are the following disturbed types of solar wind: (1) CIR (Corotating Interaction Regions) formed in compress region between slow and high‐speed streams of solar wind, (2) ICME (interplanetary coronal mass ejections including magnetic clouds and less powerful disturbance ‐ Ejecta), and (3) Sheath formed in compress region between fast ICME and slower stream of solar wind (see reviews and recent papers, for instance, by Tsurutani and Gonzalez [1997], Gonzalez et al [1999], Yermolaev and Yermolaev [2006], Zhang et al [2007], Turner et al [2009], Yermolaev et al [2010b, 2011, 2012], Nikolaeva et al [2011], Gonzalez et al [2011], and Guo et al [2011], and references therein). One of recent important experimental results is evidence that features of magnetic storm depend on type of the interplanetary driver [ Borovsky and Denton , 2006; Denton et al , 2006; Huttunen et al , 2006; Pulkkinen et al , 2007a; Plotnikov and Barkova , 2007; Longden et al , 2008; Turner et al , 2009; Yermolaev et al , 2010b, 2012; Guo et al , 2011; Buzulukova et al , 2012; Liemohn and Katus , 2012]. These facts indicate that mechanisms of magnetic storm generation (or modes of these mechanisms) can differ depending on the driver.…”