Geoeffectiveness of halo coronal mass ejections

By Nat Gopalswamy, S. Yashiro, S. Akiyama. 2007

210 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/839aa414f7fe2c4f44eaffc92aa0edd387d3ff81

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Nat Gopalswamy
2. S. Yashiro
3. T. Howard
4. R. Howard
5. D. Webb
6. A. Vourlidas
7. S. Akiyama
8. M. Temmer

In Molecular Biology

1. Nat Gopalswamy
2. T. Howard
3. D. Webb
4. A. Vourlidas
5. R. Howard
6. S. Yashiro
7. Jan Luhmann
8. S. Akiyama

Citations in the corpus

• CME interactions with coronal holes and their interplanetary consequences (2009, methodology): “…defined as the heliographic coordinates of the associated eruption: H-alpha flare location if available from the Solar Geophysical Data or the location of an associated disk activity such as EUV dimming or post eruption arcades [see Gopalswamy et al., 2007 for details on CME source identification].”
• History and development of coronal mass ejections as a key player in solar terrestrial relationship (2016, background): “Frontside halos (those originating on the Earth-facing side of the Sun) are important for space weather because they are expected to directly impact Earth as magnetic clouds (Webb et al. 2000; St. Cyr 2005; Gopalswamy et al. 2007, 2010b).”
• The SOHO/LASCO CME Catalog (2009, background): “The halo CMEs are inherently more energetic and cause geomagnetic storms when frontsided (Gopalswamy et al. 2007) even though their true width is unknown.”
• Coronal Mass Ejections: Observations (2012, methodology): “Although most flares occur independently of CMEs, the fastest, most energetic CMEs do tend to be associated with bright flares, and reported flares are associated with most frontside, full halo CMEs (e.g., Webb, 2002; Gopalswamy et al., 2007).”
• Properties of Ground Level Enhancement Events and the Associated Solar Eruptions During Solar Cycle 23 (2012, background): “Most of the CMEs were full halos (width = 360◦), which means the true width of these CMEs is unknown, but large (Gopalswamy et al. 2007).”
• Multispacecraft observation of magnetic cloud erosion by magnetic reconnection during propagation (2012, background): “…(ICMEs), are magnetized plasma structures that play a pivotal role in solar-terrestrial interaction [Gosling, 1993; Wimmer-Schweingruber et al., 2006; Borovsky and Denton, 2006; Foullon et al., 2007; Gopalswamy et al., 2007; Lavraud and Borovsky, 2008;Möstl et al., 2010; Richardson and Cane, 2010].”