A Three-dimensional Flux Rope Model for Coronal Mass Ejections Based on a Loss of Equilibrium

By Ilia I. Roussev, T. Forbes, Tamas I. Gombosi, Igor M. Sokolov, D. Dezeeuw, Juhani Birn. 2003

184 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/0c7bb22fc790af5b7c47ff745d5c9df1bb49a711

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

Citations in the corpus

MAGNETOHYDRODYNAMIC WAVES AND CORONAL HEATING: UNIFYING EMPIRICAL AND MHD TURBULENCE MODELS (2012, methodology): “In the context of solar-heliospheric physics, BATS-R-US has been utilized to model the global structure of the solar corona and solar wind (Roussev et al. 2003b; Cohen et al. 2007, 2008), as well as the initiation (Roussev et al. 2003a; Jacobs et al. 2009) and propagation of idealized (Manchester…”
The Calm before the Storm: The Link between Quiescent Cavities and Coronal Mass Ejections (2006, background): “The idea of the erupting CME as a magnetic flux rope has gained acceptance over the years (Amari et al. 2003; Chen&Krall 2003; Roussev et al. 2003; MacNeice et al. 2004; Manchester et al. 2004).”
Eruption of a Buoyantly Emerging Magnetic Flux Rope (2003, background): “When such a flux rope is fully formed in the corona, an increase in twist might further drive an eruption in one of two ways: First, an increase in the hoop force could bodily drive a flux rope from the corona, as numerically modeled by Wu et al. (1999) and Roussev et al. (2003).”
Three-dimensional MHD Simulation of the 2003 October 28 Coronal Mass Ejection: Comparison with LASCO Coronagraph Observations (2008, methodology): “This eruption generator follows from the work of Roussev et al. (2003a) who incorporated the Titov & Démoulin (1999) flux rope in the BATS-R-US code.”
Ideal kink instability of a magnetic loop equilibrium (2003, background): “…the stability of the torus with respect to global expansion (growing perturbationsδR > 0) and found instability for sufficiently large radii,R >∼ √ 2L. Roussev et al. (2003) confirmed this recently by numerical simulations, which also suggested that the instability thres - old lies near 5L and…”
Space Weather Modeling Framework: A new tool for the space science community (2005, background): “To truly extend the SWMF, one needs to define a new domain and add a new component to the framework.”
Formation of current sheets and sigmoidal structure by the kink instability of a magnetic loop (2003, unknown): “This has recently been confirmed by Roussev et al. (2003).”
Generalized Squashing Factors for Covariant Description of Magnetic Connectivity in the Solar Corona (2007, background): “…seems to be quite natural that this HFT is pinched into a vertical current sheet below the flux rope by its upward movement when the kink or torus instability is developed in the configuration at a sufficiently large twist of the field lines in the rope (Török et al. 2004; Roussev et al. 2003).”
Confined and Ejective Eruptions of Kink-unstable Flux Ropes (2005, background): “It is possible to obtain an eruptive behavior of the flux rope by removing the line current; however, such a modification leads to an infinite number of field line turns at the surface of the flux rope (Roussev et al. 2003).”
ELECTRIC CURRENTS IN FLARE RIBBONS: OBSERVATIONS AND THREE-DIMENSIONAL STANDARD MODEL (2014, background): “…the possibility of having more complicated, highly twisted, kink unstable flux ropes, as is required in some models of CME ejection (e.g., Gibson & Low 1998; Low 2001 (Figure 9); Roussev et al. 2003; Cohen et al. 2010; Kliem et al. 2010; Shiota et al. 2010; Lugaz et al. 2011; Roussev et al. 2012).”
NUMERICAL SIMULATION OF AN EUV CORONAL WAVE BASED ON THE 2009 FEBRUARY 13 CME EVENT OBSERVED BY STEREO (2009, methodology): “Simulation results were obtained using the Space Weather Modeling Framework, developed by the Center for Space Environment Modeling, at the University of Michigan with funding support from NASA ESS, NASA ESTO-CT, NSF KDI, and DoD MURI.”
The Role of Magnetic Reconnection in the Observable Features of Solar Eruptions (2004, background): “Some models (e.g., Forbes & Isenberg 1991; Gibson & Low 1998; Krall, Chen, & Santoro 2000; Wu, Guo, & Dryer 1997; Roussev et al. 2003) assume that a magnetic flux rope above the solar surface becomes unstable as a result of footpoint motion, injection of magnetic helicity, or draining of heavy…”