Properties of Interplanetary Coronal Mass Ejections

By Nat Gopalswamy. 2007

185 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/615f1f573a1262924c49592d9c4b117b23f91069

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In Astronomy and Astrophysics

Citations in the corpus

History and development of coronal mass ejections as a key player in solar terrestrial relationship (2016, background): “There is considerable evidence to support the idea that all ICMEs may be flux ropes (Marubashi 1997; Owens et al. 2005; Gopalswamy 2006; Riley et al. 2006; Gopalswamy et al. 2013a; Vourlidas et al. 2013; Marubashi et al. 2015).”
CME interactions with coronal holes and their interplanetary consequences (2009, background): “Just a decade ago, the origin of such shocks was a mystery [Schwenn, 1996], but extensive observations of CMEs and their IP counterparts over the past decade have revealed that these shocks are also CME driven but the driver does not arrive at the observer because of the observer’s location with res”
Geoeffectiveness of halo coronal mass ejections (2007, background): “[20] The CME rate and mean speed increased from solar minimum to maximum [Gopalswamy, 2006a], so one expects more halos during solar maximum.”
Solar Orbiter (2012, background): “additional aspects of the mechanism such as seed populations or shock geometry must play important roles that are not yet well understood (Gopalswamy, 2006; Desai et al., 2006; Mewaldt, 2006).”
The Solar Orbiter mission (2020, background): “By the time the particles reach 1 AU, they are so thoroughly mixed that these effects cannot be untangled (e.g. Gopalswamy 2006; Cohen et al. 2007; Gómez-Herrero et al. 2017; Klassen et al. 2018; Dresing et al. 2018; Effenberger & Petrosian 2018; He & Wan 2019).”