On the Temporal Relationship between Coronal Mass Ejections and Flares

By J. Zhang, K. Dere, R. Howard, M. Kundu, Simon D. M. White. 2001

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View Paper: https://www.semanticscholar.org/paper/b04635ceada073d4608d1a93948d6af2bd5936f6

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In Astronomy and Astrophysics

Citations in the corpus

On the Magnetic Flux Budget in Low-Corona Magnetic Reconnection and Interplanetary Coronal Mass Ejections (2007, background): “…with LASCO C1-C2-C3 data have demonstrated that the timing relationship between flares and fast CMEs is much closer than previously thought (Zhang et al. 2001; Gallagher et al. 2003; Cheng et al. 2003;Wang et al. 2003; Vrsnak et al. 2005), and the latest studies further illustrate a…”
The CME-flare relationship: Are there really two types of CMEs? (2005, background): “Furthermore, the rapid acceleration stage of CMEs is closely synchronized with the rising phase of the associated soft X-ray bursts (Zhang et al. 2001; see also Vršnak et al. 2004a, and references therein).”
Identification of Solar Sources of Major Geomagnetic Storms between 1996 and 2000 (2003, background): “…also generally called impulsive CMEs, are found to be accelerated in the lower corona within tens of minutes in time and a few solar radii in distance but often maintain a constant speed or slightly decrease speed in the outer corona (Sheeley et al. 1999; Andrews & Howard 2001; Zhang et al. 2001).”
Rapid Acceleration of a Coronal Mass Ejection in the Low Corona and Implications for Propagation (2003, methodology): “The findings of this Letter support the flare-associated CME scenario of Zhang et al. (2001), who propose a three-component kinematic evolution consisting of an initiation phase, a rapid acceleration phase, and a propagation phase.”
Cone model for halo CMEs: Application to space weather forecasting (2004, background): “Most slower CMEs accelerate as they move outward through LASCO C2 field of view and then travel with approximately constant speed in LASCO C3 field of view, while fast events have been observed to decelerate [e.g., Sheeley et al., 1999; Andrews and Howard, 2001; Zhang et al., 2001 ].”
An Observational Overview of Solar Flares (2011, background): “Further studies revealed a close correlation between the CME acceleration and the derivative of the flare SXR flux, taken as a proxy for the flare enrgy release (Zhang et al. 2001, 2004; Maričić et al. 2007).”
Sixty-five years of solar radioastronomy: flares, coronal mass ejections and Sun–Earth connection (2008, methodology): “Several large CMEs, called halo CMEs because they surround the occulting disk like a halo, have also been observed by the white-light coronagraph, Solwind on the satellite P78-1 (Howard et al. 1982).”
Processes that Promote and Deplete the Exosphere of Mercury (2007, background): “Recent studies on temporal correspondence between CMEs and flares provide arguments in favor of the so-called common-cause scenario, according to which flares and CMEs are different manifestations of the same largescale magnetic process (Zhang et al. 2001).”
Magnetic Reconnection and Mass Acceleration in Flare-Coronal Mass Ejection Events (2004, background): “…light curves and the time derivative of the soft X-ray light 3 For more information, see: http://cdaw.gsfc.nasa.gov/CME_list/. curve to infer the evolution of the magnetic reconnection rate, as in previous studies (Zhang et al. 2001; Gallagher et al. 2003; Cheng et al. 2003; Wang et al. 2003).”
A Statistical Study of Main and Residual Accelerations of Coronal Mass Ejections (2006, methodology): “2) have been reported (Zhang et al. 2001; Alexander et al. 2002; Gallagher et al. 2003).”
A Model for Spectral and Compositional Variability at High Energies in Large, Gradual Solar Particle Events (2006, background): “Wewould generally expect the nonradial expansion of CMEs (e.g., Zhang et al. 2001) to produce extensive regions of quasiperpendicular shocks on their flanks, at least out to altitudes of a few R .”
Eruption of magnetic flux ropes during flux emergence (2008, neutral): “Typically, CMEs exhibit three distinct phases (Zhang et al. 2001): an initiation phase, often observed as the slow rise of a filament (e.g. Sterling & Moore 2005; Schrijver et al. 2008), a rapid acceleration phase, and a propagation phase at approximately constant velocity.”
Dynamical and Physical Properties of a Post-Coronal Mass Ejection Current Sheet (2003, background): “Previous studies found low-coronal accelerations of as much as 2–7 km s 2 (e.g., Zhang et al. 2001; Alexander, Metcalf, & Nitta 2002).”