Prominence Eruptions and Coronal Mass Ejection: A Statistical Study Using Microwave Observations

By Nat Gopalswamy, M. Shimojo, W. Lu, S. Yashiro, K. Shibasaki, R. Howard. 2003

346 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/b857646e9b73d4e814886f25f47609b33431d959

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In Astronomy and Astrophysics

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

In Molecular Biology

1. Nat Gopalswamy
2. D. Webb
3. T. Howard
4. S. Yashiro
5. S. Akiyama
6. P. Démoulin
7. B. Vršnak
8. R. Howard

Citations in the corpus

• Geoeffectiveness of halo coronal mass ejections (2007, background): “From an observational point of view, halo CMEs are referred as full (type F), asymmetric (type A), and partial (type P) halos [Gopalswamy et al., 2003a].”
• A Global Picture of CMEs in the Inner Heliosphere (2004, background): “For these two phases, complete CME observations exist and the CME rates can be easily separated into LL and HL parts (Gopalswamy et al., 2003d).”
• Kinematics of coronal mass ejections between 2 and 30 solar radii. What can be learned about forces governing the eruption (2004, methodology): “Firstly, it is an extension of previous statistical analyses of kinematics of large samples of CMEs (e.g. Hundhausen 1993; Hundhausen et al. 1994; Harrison 1995; St. Cyr et al. 1999, 2000; Moon et al. 2002; Gopalswamy et al. 2003, and references therein).”
• Coronal Mass Ejections and Solar Polarity Reversal (2003, methodology): “Since eruptive prominences are almost always accompanied by coronal mass ejections (CMEs), one can identify the disappearance of PCFs with high-latitude (HL) CMEs (Gopalswamy et al. 2003b).”
• Solar filament eruptions and their physical role in triggering Coronal Mass Ejections (2012, background): “The rate of the association is very high according to the statistics made for different sets of events observed during the past solar cycles (56%, Jing et al., 2004; 83%, Gopalswamy et al., 2003; 92%, Hori and Culhane, 2002; 62%, Liu et al., 2012b).”
• Properties of Interplanetary Coronal Mass Ejections (2007, background): “However, prominence eruptions form the inner core of white-light CMEs (Hori and Culhane, 2002; Gopalswamy et al., 2003b) and eruptive flares are indicative of CMEs (Munro et al., 1979).”
• CME interactions with coronal holes and their interplanetary consequences (2009, background): “Using a case study [Gopalswamy et al., 2000b] and a statistical study [ Gopalswamy et al., 2003c ] it was shown that CMEs have an equatorward offset of position angle compared to that of the eruptiveprominencesource.Thenonradialmotionduringthe rise phase of the solar cycle has been attributed to the”
• A catalog of white light coronal mass ejections observed by the SOHO spacecraft (2004, background): “[16] Gopalswamy et al. [2003a, 2003c] examined the latitudes of CMEs associated with prominence eruptions and found a north-south asymmetry in the high-latitude activities.”
• Properties of Ground Level Enhancement Events and the Associated Solar Eruptions During Solar Cycle 23 (2012, methodology): “12a) reported in Gopalswamy et al. (2003), we obtained the initial height of prominences as shown in the histogram in Fig.”
• Coronal Mass Ejections: Observations (2012, background): “…seen in previous cycles and is related to observations that high latitude CMEs arise from polar crown filaments which have a “rush to the poles” near maximum and disappear (erupt) with a frequency that slightly lags sunspot numbers at low latitudes (Cliver and Webb, 1998; Gopalswamy et al., 2003b).”
• Solar source of the largest geomagnetic storm of cycle 23 (2005, methodology): “Similar constraining of CME motion by Sun’s global dipolar field and polar coronal holes have been reported before [Gopalswamy et al., 2000a, 2003].”
• History and development of coronal mass ejections as a key player in solar terrestrial relationship (2016, background): “The fact that the CME rate is correlated with sunspot number (SSN) reported from preSOHO coronagraphs (Webb and Howard 1994) was readily confirmed with SOHO CMEs for cycle 23 (Gopalswamy et al. 2003a).”