Type II radio bursts and energetic solar eruptions

By Nat Gopalswamy, E. Aguilar-Rodriguez, S. Yashiro, S. Nunes, M. Kaiser, R. Howard. 2003

155 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Oceanography

View Paper: https://www.semanticscholar.org/paper/4785f6042550009a6d36bd0ad20af880b8b2f9db

How researchers see this paper

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In Astronomy and Astrophysics

1. Nat Gopalswamy
2. M. Temmer
3. S. Yashiro
4. R. Howard
5. H. Hudson
6. A. Vourlidas
7. N. Lugaz
8. R. Schwenn

In Oceanography

1. I. Usoskin
2. Nat Gopalswamy
3. N. Lugaz
4. R. Schwenn
5. A. Vourlidas
6. E. Cliver
7. D. Hathaway
8. S. Solanki

Citations in the corpus

• Coronal mass ejections of solar cycle 23 (2006, background): “The solid curve is the empirical shock arrival (ESA) model, which relates the Sun–Earth transit time (T in hours) to the CME speed (V km s−1) by the formula, T = abV + c, where a = 151.002, b = 0.998625, and c = 11.5981 (Gopalswamy et al. 2005a).”
• The Interaction of Successive Coronal Mass Ejections: A Review (2016, background): “Note that only 15 events propagated from Sun to Earth in less than 24 hours in the past 150 years (Gopalswamy et al., 2005).”
• Coronal mass ejections and other extreme characteristics of the 2003 October–November solar eruptions (2005, background): “Not surprisingly, all the inferred speeds exceed 1500 km s � 1 , while the average speed of the historical events is � 1957 km s � 1 . Note that this speed is larger than the average speed of CMEs associated with SEP events (1446 km s � 1 ) and with type II radio bursts with counterparts in all wave”
• Space Weather: The Solar Perspective (2006, background): “…of these extraordinary Halloween events and their effects were assembled in special editions of Geophysical Research Letters and Journal of Geophysical Research (see http: //www.agu.org/journals/ss/VIOLCONN1/ and were reviewed by Veselovsky et al. (2004), (see also Gopalswamy et al., 2005b).”
• The SOHO/LASCO CME Catalog (2009, background): “CMEs can also be deflected by other CMEs and by nearby coronal holes (Gopalswamy et al. 2005a).”
• Geoeffectiveness of halo coronal mass ejections (2007, background): “Occasionally, the flux rope axes may be highly inclined to the ecliptic plane and cause either very intense storms [Gopalswamy et al., 2005a] or no storm at all [Yurchyshyn et al., 2001] depending on which way the axial field is pointed.”
• CME interactions with coronal holes and their interplanetary consequences (2009, background): “Interestingly, the same region (AR 0501) produced another halo CME two days earlier (2003 November 18) when it was at S01E33, resulting in a shock with driver (a magnetic cloud) at Earth and caused the largest geomagnetic storm of cycle 23 [see Gopalswamy et al., 2005a].”
• Estimating the frequency of extremely energetic solar events, based on solar, stellar, lunar, and terrestrial records (2012, result): “s. Kahler et al. [1978] suggested that the type II shocks associated with SEP events were driven by CMEs, a suggestion that has found increasing support [Gopalswamy et al., 2002; Cliver et al., 2004; Gopalswamy et al., 2005]. By the mid-1980s the basic two-class picture of SEP acceleration was stren”
• Properties of Ground Level Enhancement Events and the Associated Solar Eruptions During Solar Cycle 23 (2012, methodology): “Type II bursts with emission components from metric to kilometric wavelengths indicate that the driving CMEs are of the highest kinetic energy (Gopalswamy et al. 2005b).”