Magnetic Reconnection and Mass Acceleration in Flare-Coronal Mass Ejection Events

By J. Qiu, Haimin Wang, C. Cheng, D. Gary. 2004

197 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/90023d1968a6863e089dafd9b7a22353a6bb929e

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Citations in the corpus

Production of the large scale superluminal ejections of the microquasar GRS 1915+105 by violent magnetic reconnection (2005, background): “…of solar flares, considerable progress has been made in recent years towardsthe etermination of more realistic reconnection rates during flare events based mostly on the separation speed ofHα flare ribbons (e.g., Qiu et al. 2004; Jing et al. 2005; Sakajiri et al. 2004, Takasaki et al. 2004).”
The CME-flare relationship: Are there really two types of CMEs? (2005, background): “…the reconnection rate and the acceleration of the ejection was presented even more directly by Wang et al. (2003), Fletcher et al. (2004) and Qiu et al. (2004), who showed that the CME acceleration is correlated with the product of the ribbon expansion-velocity and the underlying…”
Implications of X-ray Observations for Electron Acceleration and Propagation in Solar Flares (2011, background): “…to be correlated with the rate at which magnetic flux is swept up by the expanding footpoints of flare loops and with the rate of looptop expansion (Qiu et al. 2004; Sui et al. 2004; Holman 2005), indicating that the electron acceleration rate is correlated with the rate of magnetic reconnection.”
Non-commercial Research and Educational Use including without Limitation Use in Instruction at Your Institution, Sending It to Specific Colleagues That You Know, and Providing a Copy to Your Institution's Administrator. All Other Uses, Reproduction and Distribution, including without Limitation Comm (2005, unknown): “Later, the Cosenza group in Italy achieved some notable successes, despite the need for significant operator intervention to avoid the problem of trapping in local minima [10,11].”
A Statistical Study of Main and Residual Accelerations of Coronal Mass Ejections (2006, methodology): “Individual events with normal accelerations have been reported by many studies (Wood et al. 1999; Shanmugaraju et al. 2003; Qiu et al. 2004; Vršnak et al. 2004; Kundu et al. 2004; Sterling & Moore 2005).”
Direct Observations of the Magnetic Reconnection Site of an Eruption on 2003 November 18 (2005, background): “…indirectly by observing the dynamic behavior of the products of magnetic reconnection: the separating flare ribbons on the solar surface (Poletto & Kopp 1986; Qiu et al. 2002; Wang et al. 2003; Qiu et al. 2004), the growing flare loops in the corona (Sui & Holman 2003; Sui et al. 2004), and so on.”
Topological Evolution of a Fast Magnetic Breakout CME in Three Dimensions (2008, background): “For example, Qiu et al. (2004) measured an erupting filament peak acceleration of 3000 m s 2, St. Cyr et al. (1999) observed a peak acceleration of 3270 m s 2, and Alexander et al. (2002) and Gallagher et al. (2003) found erupting X-ray and EUV features having maximum acceleration on the order of…”
On the Magnetic Flux Budget in Low-Corona Magnetic Reconnection and Interplanetary Coronal Mass Ejections (2007, background): “The magnetic reconnection rate has been inferred from flare observations by a number of research groups (Poletto & Kopp 1986; Isobe et al. 2002, 2005; Fletcher & Hudson 2001; Qiu et al. 2002, 2004; Fletcher et al. 2004; Qiu & Yurchyshyn 2005; Saba et al. 2006).”