Modeling the Initiation of the 2006 December 13 Coronal Mass Ejection in Ar 10930: The Structure and Dynamics of the Erupting Flux Rope

Fan, Yuhong

doi:10.3847/0004-637x/824/2/93

Cited by 26 publications

(34 citation statements)

References 25 publications

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“…Emerging flux, possibly evolving into flux rope formation, is thought to play a crucial role in supplying free magnetic energy into the AR corona as an energy source for flares and coronal mass ejections (e.g. Fan, 2005;Kazachenko et al, 2015;Fan, 2016), as well as in triggering these events (e.g. Chen and Shibata, 2000;Kusano et al, 2012;Park et al, 2013;Ding, 2015, 2016).…”

Section: Summary and Discussionmentioning

confidence: 99%

Photospheric Shear Flows in Solar Active Regions and Their Relation to Flare Occurrence

et al. 2018

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Solar active regions (ARs) that produce major flares typically exhibit strong plasma shear flows around photospheric magnetic polarity inversion lines (MPILs). It is therefore important to quantitatively measure such photospheric shear flows in ARs for a better understanding of their relation to flare occurrence. Photospheric flow fields were determined by applying the Differential Affine Velocity Estimator for Vector Magnetograms (DAVE4VM) method to a large data set of 2,548 co-aligned pairs of AR vector magnetograms with 12-min separation over the period 2012-2016. From each AR flow-field map, three shearflow parameters were derived corresponding to the mean (< S >), maximum (S max ) and integral (S sum ) shear-flow speeds along strong-gradient, strong-field MPIL segments. We calculated flaring rates within 24 hr as a function of each shear-flow parameter, and also investigated the relation between the parameters and the waiting time (τ ) until the next major flare (class M1.0 or above) after the parameter observation. In general, it is found that the larger S sum an AR has, the more likely it is for the AR to produce flares within 24 hr. It is also found that among ARs which produce major flares, if one has a larger value of S sum then τ generally gets shorter. These results suggest that large ARs with widespread and/or strong shear flows along MPILs tend to not only be more flare productive, but also produce major flares within 24 hr or less.

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Section: Summary and Discussionmentioning

confidence: 99%

Photospheric Shear Flows in Solar Active Regions and Their Relation to Flare Occurrence

et al. 2018

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“…Specifically, out-of-equilibrium flux ropes, due to their immediate expansion, may not well reproduce the frequently observed, B z -relevant rotation of CMEs about their rise direction (e.g., Démoulin 2008; Thompson et al 2012). This is particularly true for cases in which most of the rotation occurs low in the corona, while the ejected flux is still accelerating (e.g., Török et al 2010;Kliem et al 2012;Fan 2016). Furthermore, inserting a flux rope into a background corona inevitably triggers an unphysical, wave-like perturbation of the system, which superimposes with the modeled CME if the latter starts immediately.…”

Section: Introductionmentioning

confidence: 94%

Sun-to-Earth MHD Simulation of the 2000 July 14 “Bastille Day” Eruption

Török¹,

Downs²,

Linker³

et al. 2018

ApJ

159

114

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Solar eruptions are the main driver of space-weather disturbances at the Earth. Extreme events are of particular interest, not only because of the scientific challenges they pose, but also because of their possible societal consequences. Here we present a magnetohydrodynamic (MHD) simulation of the 14 July 2000 "Bastille Day" eruption, which produced a very strong geomagnetic storm. After constructing a "thermodynamic" MHD model of the corona and solar wind, we insert a magnetically stable flux rope along the polarity inversion line of the eruption's source region and initiate the eruption by boundary flows. More than 10 33 ergs of magnetic energy are released in the eruption within a few minutes, driving a flare, an EUV wave, and a coronal mass ejection (CME) that travels in the outer corona at ≈ 1500 km s −1 , close to the observed speed. We then propagate the CME to Earth, using a heliospheric MHD code. Our simulation thus provides the opportunity to test how well in situ observations of extreme events are matched if the eruption is initiated from a stable magnetic-equilibrium state. We find that the flux-rope center is very similar in character to the observed magnetic cloud, but arrives ≈ 8.5 hours later and ≈ 15 • too far to the North, with field strengths that are too weak by a factor of ≈ 1.6. The front of the flux rope is highly distorted, exhibiting localized magnetic-field concentrations as it passes 1 AU. We discuss these properties with regard to the development of space-weather predictions based on MHD simulations of solar eruptions.

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“…Starting from analytical flux-rope models, Fan and Gibson (2004) and Török and Kliem (2005) reported similarly large rotations (up to 120°) as a result of the same instability. Using a similar flux-rope model, Fan (2016) obtained an even larger rotation of almost 180°, i.e., a full reversal of the magnetic field vector at the front of the flux rope, in a recent simulation of the 13 December 2006 event. Isenberg and Forbes (2007) suggested that the presence of an external shear field surrounding a pre-eruptive flux rope (i.e., of an ambient field component pointing along the axis of the rope) provides a different mechanism for the rotation of a flux rope, once the rope leaves its equilibrium state and rises in the corona.…”

Section: Cme Rotationmentioning

confidence: 99%

“…Many models use observed magnetograms as boundary condition for the magnetic field at the lower boundary, and recently observed surface flows have been included as well (Jiang et al 2016). Some simulations restrict the calculation to the evolution in the corona (e.g., Zuccarello et al 2012b;Amari et al 2014;Fan 2016), while others model the propagation of the ejecta to 1 AU but do not include the coronal evolution. Instead, the latter models start the simulation in the inner heliosphere (typically at around 20-30 R ) and use for the initial ICME some idealized model whose parameters are chosen guided by coronagraph observations (e.g., Shiota and Kataoka 2016).…”

Section: Modeling Cmes From Sun To Earth: the Bastille Day Eventmentioning

confidence: 99%

The Physical Processes of CME/ICME Evolution

et al. 2017

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As observed in Thomson-scattered white light, coronal mass ejections (CMEs) are manifest as large-scale expulsions of plasma magnetically driven from the corona in the most energetic eruptions from the Sun. It remains a tantalizing mystery as to how these erupting magnetic fields evolve to form the complex structures we observe in the solar wind at Earth. Here, we strive to provide a fresh perspective on the post-eruption and interplanetary evolution of CMEs, focusing on the physical processes that define the many complex interactions of the ejected plasma with its surroundings as it departs the corona and propagates through the heliosphere. We summarize the ways CMEs and their interplanetary CMEs (ICMEs) are rotated, reconfigured, deformed, deflected, decelerated and disguised during their journey through the solar wind. This study then leads to consideration of how structures originating in coronal eruptions can be connected to their far removed interplanetary counterparts. Given that ICMEs are the drivers of most geomagnetic storms (and the sole driver of extreme storms), this work provides a guide to the processes that must be considered in making space weather forecasts from remote observations of the corona.

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Modeling the Initiation of the 2006 December 13 Coronal Mass Ejection in Ar 10930: The Structure and Dynamics of the Erupting Flux Rope

Cited by 26 publications

References 25 publications

Photospheric Shear Flows in Solar Active Regions and Their Relation to Flare Occurrence

Photospheric Shear Flows in Solar Active Regions and Their Relation to Flare Occurrence

Sun-to-Earth MHD Simulation of the 2000 July 14 “Bastille Day” Eruption

The Physical Processes of CME/ICME Evolution

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