Inverse and normal coronal mass ejections: evolution up to 1 AU

Chané, Emmanuel; Holst, B. van der; Jacobs, Carla; Poedts, Stefaan; Kimpe, Dries

doi:10.1051/0004-6361:20053802

Cited by 54 publications

(63 citation statements)

References 15 publications

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“…These authors distinguish 'normal' and 'inverse' prominences based on their orientation with respect to the background field, and find that the normal variant is more likely to erupt. This finding has been confirmed numerically by Chané et al (2006), see Section 3.1. 2.…”

Section: Model Classificationssupporting

confidence: 68%

“…The first is to ignore the misalignment of expansion direction and magnetic symmetry axis and to assume cylindrical symmetry anyway (e.g. Chané et al, 2006). This implies a closed, torus-shaped CME geometry which is not anchored on the Sun, a configuration that could potentially be relevant for tube-shaped magnetic clouds.…”

Section: Numerical Mhd Propagation Modelsmentioning

confidence: 99%

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4π Models of CMEs and ICMEs (Invited Review)

Kleimann¹

2012

Sol Phys

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Coronal mass ejections (CMEs), which dynamically connect the solar surface to the far reaches of interplanetary space, represent a major manifestation of solar activity. They are not only of principal interest but also play a pivotal role in the context of space weather predictions. The steady improvement of both numerical methods and computational resources during recent years has allowed for the creation of increasingly realistic models of interplanetary CMEs (ICMEs), which can now be compared to high-quality observational data from various space-bound missions. This review discusses existing models of CMEs, characterizing them by scientific aim and scope, CME initiation method, and physical effects included, thereby stressing the importance of fully 3-D ('4π') spatial coverage.

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Section: Model Classificationssupporting

confidence: 68%

Section: Numerical Mhd Propagation Modelsmentioning

confidence: 99%

4π Models of CMEs and ICMEs (Invited Review)

Kleimann¹

2012

Sol Phys

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“…Relaxation of the uniform density 2 http://lasco-www.nrl.navy.mil/cmelist.html assumption may increase the size estimate significantly if we also assume that the light path passes through the densest part of a CME. Even though CMEs are quite large in angular extent, simulations show that they retain a small dense core (Chané et al 2006). Furthermore, the effect from CMEs on the light time delay will be largest close to conjunction, since the CMEs are then closer to the Sun when they interfere with the radio transmission.…”

Section: Variation Of the Pioneer Anomalymentioning

confidence: 99%

The constancy of the Pioneer anomalous acceleration

Olsen

2006

A&A

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Aims. The temporal evolution of the Pioneer anomalous acceleration is studied to determine its correlation with solar activity. Methods. Bayesian Weighted Least Squares algorithms and Kalman filters are used to study the temporal evolution of the Pioneer anomalous acceleration. Doppler data for Pioneer 10 and 11 spanning respectively 11 and 3.5 years were used in this study. Results. The Doppler data itself can not be used to distinguish between a constant acceleration model and acceleration proportional to the remaining plutonium in the radioisotope thermoelectric generators. There are significant short term variations in the anomalous acceleration. These are shown to be consistent with radio plasma delay from coronal mass ejections.

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“…Flux rope evolution has also been investigated with MHD simulations (Cargill et al 2000;Cargill & Schmidt 2002;Riley et al 2003;Manchester et al 2004;Chané et al 2006;Shen et al 2007). A flux rope model is typically inserted in a SW model close to the Sun as an initial condition.…”

Section: Introductionmentioning

confidence: 99%

Causes and consequences of magnetic cloud expansion

Démoulin¹,

Dasso

2009

A&A

147

191

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Context. A magnetic cloud (MC) is a magnetic flux rope in the solar wind (SW), which, at 1 AU, is observed ∼2-5 days after its expulsion from the Sun. The associated solar eruption is observed as a coronal mass ejection (CME). Aims. Both the in situ observations of plasma velocity distribution and the increase in their size with solar distance demonstrate that MCs are strongly expanding structures. The aim of this work is to find the main causes of this expansion and to derive a model to explain the plasma velocity profiles typically observed inside MCs. Methods. We model the flux rope evolution as a series of force-free field states with two extreme limits: (a) ideal magnetohydrodynamics (MHD) and (b) minimization of the magnetic energy with conserved magnetic helicity. We consider cylindrical flux ropes to reduce the problem to the integration of ordinary differential equations. This allows us to explore a wide variety of magnetic fields at a broad range of distances to the Sun. Results. We demonstrate that the rapid decrease in the total SW pressure with solar distance is the main driver of the flux-rope radial expansion. Other effects, such as the internal over-pressure, the radial distribution, and the amount of twist within the flux rope have a much weaker influence on the expansion. We demonstrate that any force-free flux rope will have a self-similar expansion if its total boundary pressure evolves as the inverse of its length to the fourth power. With the total pressure gradient observed in the SW, the radial expansion of flux ropes is close to self-similar with a nearly linear radial velocity profile across the flux rope, as observed. Moreover, we show that the expansion rate is proportional to the radius and to the global velocity away from the Sun. Conclusions. The simple and universal law found for the radial expansion of flux ropes in the SW predicts the typical size, magnetic structure, and radial velocity of MCs at various solar distances.

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Inverse and normal coronal mass ejections: evolution up to 1 AU

Cited by 54 publications

References 15 publications

4π Models of CMEs and ICMEs (Invited Review)

4π Models of CMEs and ICMEs (Invited Review)

The constancy of the Pioneer anomalous acceleration

Causes and consequences of magnetic cloud expansion

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