Characteristics of coronal mass ejections associated with long-wavelength type II radio bursts

By Nat Gopalswamy, S. Yashiro, M. Kaiser, R. Howard, J. Bougeret. 2001

211 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/7a73135d172e05dd8ff2a32454fb8d79fce50aef

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In Astronomy and Astrophysics

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

Citations in the corpus

• A catalog of white light coronal mass ejections observed by the SOHO spacecraft (2004, background): “Similar correlation (r = 0.44) was reported earlier for CMEs associated with decameter-hectometric (DH) radio bursts [ Gopalswamy et al., 2001a ].”
• Type II radio bursts and energetic solar eruptions (2003, background): “…in the low corona is typically small, so CMEs with slightly above average energies can become superAlfvenic to produce m type II bursts [see, e.g., Gopalswamy et al., 2001a]: once the CME speed exceeds the local Alfvenic speed, a metric type II burst is produced, irrespective of how high the CME…”
• Coronal mass ejections of solar cycle 23 (2006, background): “The CME acceleration over the entire Sun–Earth distance also has a similar relation to the CME initial speed (Gopalswamy et al. 2001b): a = −0.0054 (v − 406).”
• Space weather: the solar perspective (2021, methodology): “It is well known that CMEs during their propagation phase tend to get adjusted to the ambient solar wind flow owing to the drag force exerted by the ambient solar wind (Gopalswamy et al. 2001a; Wang et al. 2004).”
• Coronal mass ejections, type II radio bursts, and solar energetic particle events in the SOHO era (2008, background): “This is in addition to the radial variation discussed by Mann et al. (1999), Gopalswamy et al. (2001a), and Mann et al. (2003).”
• Kinematics of coronal mass ejections between 2 and 30 solar radii. What can be learned about forces governing the eruption (2004, background): “The slopes from Gopalswamy et al. (2000) and Gopalswamy et al. (2001b) are drawn at R = 40 and R = 46, respectively, corresponding to the geometrical mean (see the argumentation in Vršnak 2001a) of the considered distance ranges (0.76 and 1 au, respectively).”
• Dynamical and Physical Properties of a Post-Coronal Mass Ejection Current Sheet (2003, background): “…studies of individual CME events and statistical studies of the CME properties (e.g., Howard et al. 1985; Hundhausen, Burkepile, & St. Cyr 1994; Goldstein, Newgebauer, & Clay 1998; Innes et al. 1999; St. Cyr et al. 1999, 2000; Ciaravella et al. 2000; Akmal et al. 2001; Gopalswamy et al. 2001).”
• Coronal mass ejections and other extreme characteristics of the 2003 October–November solar eruptions (2005, methodology): “On the basis of IP type II burst association, Gopalswamy et al. [2001b] had designated CMEs with speeds � 900 km s � 1 as fast CMEs.”
• The SOHO/LASCO CME Catalog (2009, background): “The 900 km/s is not a magic number: it is based on the average speed of CMEs that produce interplanetary type II radio bursts (Gopalswamy et al. 2001b).”
• A Statistical Study of Two Classes of Coronal Mass Ejections (2002, methodology): “Extensive discussions on the interaction between CMEs and the solar wind are presented in Gopalswamy et al. (2000, 2001a).”
• Processes that Promote and Deplete the Exosphere of Mercury (2007, result): “It is also consistent with the results of other veloc- ity measurement techniques applied to separate CME phenomena (Lindsay et al. 1999; Gopalswamy et al. 2001a, 2001b, 2004; Lara et al. 2004).”
• Band-splitting of coronal and interplanetary type II bursts - III. Physical conditions in the upper corona and interplanetary space (2004, methodology): “The behaviour of the magnetosonic speed in the ARcorona that is described in the last item was anticipated by Gopalswamy et al. (2001a) and Mann et al. (2003).”
• Coronal Shocks and Solar Energetic Proton Events (2004, background): “…types of coronal shocks, one primarily observed only in the metric range (identified by the above authors with flare blast waves) and the other characteristically observed in the DH range (generally interpreted in terms of CME-driven shocks [Gopalswamy et al. 2000, 2001b; Lara et al. 2003]).”
• Properties of Ground Level Enhancement Events and the Associated Solar Eruptions During Solar Cycle 23 (2012, methodology): “Gopalswamy et al. (2005c) obtained an empirical relation between the shock travel time (T in h) to 1 AU and the near-Sun CME speed (V in km/s) using an average interplanetary acceleration (Gopalswamy et al. 2001a).”
• Prominence Eruptions and Coronal Mass Ejection: A Statistical Study Using Microwave Observations (2003, unknown): “1c) profiles were found, somewhat similar to the profiles of white-light CMEs (Gopalswamy et al. 2001).”
• Intensity variation of large solar energetic particle events associated with coronal mass ejections (2004, methodology): “This is consistent with the observed DH radio emission enhancement for a duration corresponding to the transit time of the primary shock through the density enhancement of a preceding CME observed by LASCO [Gopalswamy et al., 2001b; 2002b].”