A Statistical Study of Two Classes of Coronal Mass Ejections

By Y. Moon, G. Choe, Haimin Wang, Young-deuk Park, Nat Gopalswamy, Guo Yang, S. Yashiro. 2002

202 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/b57ca8c0a327b6684b4e811836bf92b99f436492

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. M. Temmer
2. Nat Gopalswamy
3. B. Vršnak
4. S. Yashiro
5. R. Schwenn
6. N. Lugaz
7. S. Akiyama
8. R. Howard

In Molecular Biology

1. Nat Gopalswamy
2. M. Temmer
3. S. Yashiro
4. R. Schwenn
5. S. Akiyama
6. B. Vršnak
7. R. Howard
8. N. Lugaz

Citations in the corpus

• Rapid Acceleration of a Coronal Mass Ejection in the Low Corona and Implications for Propagation (2003, background): “It is well known that CMEs are associated with both filament eruptions and solar flares (Zhang et al. 2002; Moon et al. 2002), but the driver mechanism remains elusive.”
• COMBINED STEREO/RHESSI STUDY OF CORONAL MASS EJECTION ACCELERATION AND PARTICLE ACCELERATION IN SOLAR FLARES (2010, background): “Statistical studies comparing the flare SXR peak flux and CME peak velocity find a linear correlation coefficient of about r ∼0.47 which is not very strong (Moon et al. 2002).”
• The Physical Processes of CME/ICME Evolution (2017, background): “This acceleration/deceleration tendency is already observable in the upper corona (Moon et al. 2002; Vršnak et al. 2004) and was found by comparing the distribution of coronagraphic CME velocities with the ICME speeds measured in situ at 1 AU (Gopalswamy et al. 2000, 2001b).”
• A Statistical Study of Main and Residual Accelerations of Coronal Mass Ejections (2006, background): “The continuous distribution of CME kinematic properties is not consistent with the speculation that there may be two distinct classes of CMEs: impulsive CMEs and gradual CMEs (Sheeley et al. 1999; Andrews & Howard 2001; Moon et al. 2002; Zhang et al. 2002).”
• Acceleration in Fast Halo CMEs and Synchronized Flare HXR Bursts (2008, unknown): “In statistical studies the CME velocity was found to be related with the SXR peak flux (e.g., Moon et al. 2002; Burkepile et al. 2004; Vršnak et al. 2005).”
• Visibility of coronal mass ejections as a function of flare location and intensity (2005, background): “…many researchers (Munro et al. [1979]; see Kahler [1992] for reviews), and it has been established that the CMEs associated with large X-ray flares are likely to be fast and wide [Gosling et al., 1976; MacQueen and Fisher, 1983; Kahler et al., 1989; Burkepile et al., 1994, 2004; Moon et al., 2002].”
• Kinematics of coronal mass ejections between 2 and 30 solar radii. What can be learned about forces governing the eruption (2004, methodology): “1b, can be found in the paper by Moon et al. (2002), or Ruždjak et al. (2004).”
• The CME-flare relationship: Are there really two types of CMEs? (2005, background): “A similar trend was also reported by Moon et al. (2002), however, our mean velocities are somewhat larger and our decelerations are weaker.”
• The association of coronal mass ejections with their effects near the Earth (2005, background): “Some authors claim that there are two kinds of coronal mass ejections (e.g. Sheeley et al., 1999; Srivastava et al., 2000, see alsǒSvestka, 2001; Moon et al., 2002): 1) gradual CMEs, with balloon-like shapes, accelerating slowly and over large distances to speeds in the range 300 to 600 km/s, and 2)”
• The Interaction of Successive Coronal Mass Ejections: A Review (2016, unknown): “…eruptions (see, e.g., Richardson, 1951, Fritzova-Svestkova, Chase, and Svestka, 1976, Pearce and Harrison, 1990, Biesecker and Thompson, 2000, Wang et al., 2001, Moon et al., 2002, Schrijver and Title, 2011, Jiang et al., 2011, Shen, Liu, and Su, 2012, Yang et al., 2012, Wang et al., 2016).”
• Ultraviolet spectroscopy of the extended solar corona (2006, background): “…into slower, gradually accelerating events and faster events that seem to reach constant speed by the time they are observed with coronagraphs (e.g., Sheeley et al. 1999; Moon et al. 2002), recent results suggest a more continuous distribution (Vourlidas & Patsourakos 2004; Yurchyshyn et al. 2005).”
• Space Weather: The Solar Perspective (2006, background): “Some authors claim that there are two (or more) kinds of coronal mass ejections (e.g. Sheeley Jr et al., 1999; Srivastava et al., 1999a,b; Švestka, 2001; Moon et al., 2002): (1) Gradual CMEs, with balloon-like shapes, accelerating slowly and over large distances to speeds in the range 300 to 600 km/”