Intensity variation of large solar energetic particle events associated with coronal mass ejections

By Nat Gopalswamy, S. Yashiro, S. Krucker, Guillermo Stenborg, R. Howard. 2004

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In Astronomy and Astrophysics

Citations in the corpus

Coronal mass ejections, type II radio bursts, and solar energetic particle events in the SOHO era (2008, background): “, 2004; Kahler and Vourlidas, 2005), preceding CMEs (Gopalswamy et al. 2004; Kahler 2001), which increase the efficiency of particle acceleration.”
CME interactions with coronal holes and their interplanetary consequences (2009, background): “Such deflections can move a CME closer to the Sun-Earth line [Gopalswamy et al., 2005a] or away from it [ Gopalswamy et al., 2004 ] depending on the relative location of the CH and the CME source with respect to the observer.”
Geoeffectiveness of halo coronal mass ejections (2007, background): “Sometimes multiple CMEs merge to form a single halo CME especially when the eruptions occur in quick succession from the same active region (see examples given in the work of Gopalswamy et al. [2004] ).”
Properties of Ground Level Enhancement Events and the Associated Solar Eruptions During Solar Cycle 23 (2012, background): “Since the active regions in which the GLEs occurred were prolific producers of flares and CMEs (Gopalswamy et al. 2004), the flare onsets have to be carefully examined to separate the preceding events from the GLE-associated flares.”
EUV WAVE REFLECTION FROM A CORONAL HOLE (2009, background): “Examination of the coronal dimming in the vicinity of the active region shows that most of the motion was to the west of the active region, which may be a confining effect that the eastern coronal holes had on the eruption (Gopalswamy et al., 2004).”
Type II radio bursts and energetic solar eruptions (2003, background): “This is not surprising because the speed and width distribution of CMEs associated with SEP events [Gopalswamy et al., 2004] and m-to-km type II bursts (see Figure 4) are nearly identical.”
History and development of coronal mass ejections as a key player in solar terrestrial relationship (2016, background): “Higher SEP intensity results when there is CME–CME interaction (Gopalswamy et al. 2004) and the arrival of CMEs at 1 AU gets delayed when they interact with preceding CMEs (Manoharan et al.”
> 25 MeV Proton Events Observed by the High Energy Telescopes on the STEREO A and B Spacecraft and/or at Earth During the First ∼ Seven Years of the STEREO Mission (2014, background): “…particle acceleration by multiple shocks (e.g., Pomerantz and Duggal, 1974; Levy, Duggal and Pomerantz, 1976; Cliver and Kallenrode, 2001) or multiple CMEs (e.g., Gopalswamy et al., 2002; Gopalswamy et al., 2004; Li SOLA: multiscsep6_fin.tex; 24 March 2014; 14:42; p. 23 et al., 2012) to take place.”
Solar source of the largest geomagnetic storm of cycle 23 (2005, methodology): “A low-latitude coronal hole had similarly constrained a disk center CME (2000 August 9 at 10:30 UT) to the western hemisphere (Gopalswamy et al., 2004).”
Coronal mass ejections and other extreme characteristics of the 2003 October–November solar eruptions (2005, methodology): “These regions were listed in the work of Gopalswamy et al. [2004b] for the period 1996– 2002.”
The Two Sources of Solar Energetic Particles (2012, background): “Several authors have suggested that particle acceleration is enhanced by the presence of a previous CME or SEP event (Kahler, 2001; Gopalswamy et al., 2002, 2004; Cliver, 2006; Li et al. 2012).”
GLOBAL ENERGETICS OF THIRTY-EIGHT LARGE SOLAR ERUPTIVE EVENTS (2012, background): “According to Figure 8 of Gopalswamy et al. (2004), only 16 CMEs observed from 1997 – 2002 had kinetic energy >1.4×1032 ergs.”
Coronal mass ejections of solar cycle 23 (2006, background): “4.2 SEPeffective CMEs The gradual SEP events are thought to originate from CME-driven shocks (Reames 1999; Kahler 2001; Gopalswamy et al. 2003c; 2004).”
Advances in Observing Various Coronal EUV Waves in the SDO Era and Their Seismological Applications (Invited Review) (2014, unknown): “In addition, the passage of a shock or CME (e.g. Gopalswamy et al., 2004) can modify the magnetic and plasma conditions and thus the fast-magnetosonic speed [vf ] at which a reflected wave will travel.”
The Wide-Field Imager for Solar Probe Plus (WISPR) (2014, background): “Some works have focused on the role of the variations of the environment through which the CME shocks and particles propagate (Gopalswamy et al. 2004; Kahler and Vourlidas 2005, 2013).”