A Global Picture of CMEs in the Inner Heliosphere

By Nat Gopalswamy. 2004

155 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

The SOHO/LASCO CME Catalog (2009, background): “Although information on CMEs has been available sporadically since their discovery in the early 1970s, it is only after the advent of the SOHO mission that we have continuous and uniform data on CMEs (see Gopalswamy 2004 for a review).”
CME interactions with coronal holes and their interplanetary consequences (2009, background): “Moreover, the flow speed may be much smaller than the CME speeds at least for the events we have considered [halo CMEs are inherently energetic, see Gopalswamy, 2004].”
History and development of coronal mass ejections as a key player in solar terrestrial relationship (2016, methodology): “The average speed of the general population is ~450 km/s, which is essentially the same as what was obtained using all pre-SOHO data (Gopalswamy 2004).”
Coronal mass ejections, type II radio bursts, and solar energetic particle events in the SOHO era (2008, background): “The corresponding CME kinetic energy is ∼3.3×1030 erg, which is slightly above the average kinetic energy of all CMEs (Gopalswamy, 2004).”
Geoeffectiveness of halo coronal mass ejections (2007, background): “: GEOEFFECTIVENESS OF HALO CMES 7 of 13 A06112 phase lag [Gopalswamy, 2004].”
Visibility of coronal mass ejections as a function of flare location and intensity (2005, background): “Since the main drivers of large geomagnetic storms are halo CMEs [Webb et al., 2000; Zhang et al., 2003; Gopalswamy, 2004], which is an energetic population, invisible CMEs may not produce geomagnetic storms by themselves; however, the invisible CMEs may contribute to complex geomagnetic storms…”
AUTOMATED LASCO CME CATALOG FOR SOLAR CYCLE 23: ARE CMEs SCALE INVARIANT? (2008, result): “These findings are consistent with earlier observations from past cycles (Hundhausen 1993; Howard et al. 1986) and observations of current cycle (Gopalswamy 2004).”
Space Weather: The Solar Perspective (2006, background): “, 2002; Gopalswamy, 2004). Yashiro et al. (2004) have assembled a huge catalog of more than 10,000 CMEs (by now, still counting) ever registered by the SOHO instruments over the last 10 years. For each event they present important information (e.g., images taken by the EIT and LASCO instruments, ani”
Coronal mass ejections of solar cycle 23 (2006, background): “The measured sky-plane speed ranges from a few km s−1 to ∼3000 km s−1 (see e.g., Gopalswamy 2004; Yashiro et al. 2004), with an average value of ∼483 km s−1.”
The Interaction of Successive Coronal Mass Ejections: A Review (2016, background): “This is in contradiction to the events studied in Gopalswamy (2004) and Ding et al. (2013) for which no association of larger SEP events with > 2 MeV backgrounds is found.”
Properties of Interplanetary Coronal Mass Ejections (2007, background): “The white light CMEs observed near the Sun are typically 10 times more abundant than the ICMEs observed in situ (Gopalswamy, 2004).”
Intensity variation of large solar energetic particle events associated with coronal mass ejections (2004, methodology): “The preceding eruptions were clearly observed in the inner coronal images such as from SOHO/EIT, Yohkoh/SXT and the Nobeyama Radioheliograph D R A F T August 24, 2004, 7:53pm D R A F T [Gopalswamy, 2004a].”
Coronal Mass Ejections: Observations (2012, methodology): “This pattern including the match between CMEs, prominence eruptions and the HCS has been confirmed with the LASCO data (Figure 11 – Gopalswamy, 2004; Gopalswamy et al., 2010a).”