Effects of reconnection on the coronal mass ejection process

By J. Lin, T. Forbes. 2000

532 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/a0992c570dcd819215e30c97f3fc5c499540ce5c

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In Astronomy and Astrophysics

Citations in the corpus

Evidence for the Formation of a Large-Scale Current Sheet in a Solar Flare (2003, background): “Lin & Forbes (2000) and Lin (2002) claimed that a current sheet develops following the onset of the eruption.”
Direct Observations of the Magnetic Reconnection Site of an Eruption on 2003 November 18 (2005, background): “Generally, the timescale of magnetic dissipation or reconnection is long compared with that of the catastrophe, which is the Alfvén timescale, so the development of a long current sheet is expected during major eruptions (Lin & Forbes 2000; Forbes & Lin 2000; Lin 2002).”
On the Temporal Relationship between Coronal Mass Ejections and Flares (2001, methodology): “The Ñux-rope models, which relate the CME to two-ribbon Ñares or post-Ñare loops (Forbes & Priest 1995 ; Amari et al. 2000 ; Lin & Forbes 2000), usually require spatial symmetry between CMEs and Ñares.”
A Statistical Study of Main and Residual Accelerations of Coronal Mass Ejections (2006, background): “These models usually show a transition from slow to fast motion of the erupting magnetic structure (Mikic & Linker 1994; Lin & Forbes 2000; Chen & Shibata 2000; MacNeice et al. 2004).”
Sixty-five years of solar radioastronomy: flares, coronal mass ejections and Sun–Earth connection (2008, methodology): “55 from (Schwenn et al. 2006a) and derived from the model of Lin and Forbes (2000).”
Elemental Abundances and Post-Coronal Mass Ejection Current Sheet in a Very Hot Active Region (2002, methodology): “As Lin & Forbes (2000) give the most detailed treatment of the flux rope, we compare the UVCS observations with their models.”
Dynamical and Physical Properties of a Post-Coronal Mass Ejection Current Sheet (2003, background): “…and dynamical properties, and model their propagation in the heliosphere (e.g., Mikić & Linker 1994; Chen 1996; Antiochos, DeVore, & Klimchuk 1999; Amari et al. 2000; Lin & Forbes 2000; Low 2001; Riley et al. 2002; Manchester et al. 2003; for reviews, see, e.g., Wu, Andrews, & Plunkett 2001).”
The standard flare model in three dimensions II: upper limit on solar flare energy (2012, background): “For the latter, the standard model attributes the flare energy release to magnetic reconnection that occurs in the wake of coronal mass ejections (Shibata et al. 1995; Lin & Forbes 2000; Moore et al. 2001; Priest & Forbes 2002).”
ELECTRIC CURRENTS IN FLARE RIBBONS: OBSERVATIONS AND THREE-DIMENSIONAL STANDARD MODEL (2014, background): “In models of eruptive flares, a current sheet builds up below the flux rope (e.g., Lin & Forbes 2000 and references therein).”
Magnetic Reconnection and Mass Acceleration in Flare-Coronal Mass Ejection Events (2004, background): “Recently, theoretical calculations by Lin & Forbes (2000) and numerical simulations by Cheng et al. (2003), although based on different models, both show that enhanced mass acceleration is accompanied by an enhanced magnetic reconnection rate in terms of the electric field inside the RCS.”
COMBINED STEREO/RHESSI STUDY OF CORONAL MASS EJECTION ACCELERATION AND PARTICLE ACCELERATION IN SOLAR FLARES (2010, background): “Reeves (2006) studied the relationship between the CME acceleration and the thermal energy release rate in a loss-of-equilibrium flux rope model (cf. Lin & Forbes 2000; Lin 2002).”
A Three-dimensional Flux Rope Model for Coronal Mass Ejections Based on a Loss of Equilibrium (2003, background): “As seen in Figure 2, the slope of the speed curve for the O-point is initially shallow, just as expected for a loss of equilibrium (Lin & Forbes 2000).”
The Role of Magnetic Reconnection in the Observable Features of Solar Eruptions (2004, methodology): “For B0 ¼ 100 G, at the time when h ¼ l ¼ L, Ĩ is given by equation (18) of Lin & Forbes (2000), and we find that Ĩ ¼ 0:92.”
Coronal Mass Ejections: Observations (2012, methodology): “This “standard” flare model has been developed and refined over the last few decades and has become known as Flux Cancellation or the Catastrophe model (e.g., Švestka and Cliver, 1992; Shibata et al., 1995; Lin and Forbes, 2000; Lin, 2004).”