A Time‐dependent Three‐dimensional Magnetohydrodynamic Model of the Coronal Mass Ejection

Gibson, S. E.; Low, B. C.

doi:10.1086/305107

Cited by 300 publications

(393 citation statements)

References 44 publications

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“…In this paper we propose some possible physical answers to these important questions on CME structures, based on an analytic a-D MHD model [Gibson and Low, 1998]. This model has successfully captured many aspects of limb CMEs in previous studies, and we now take the next step to show that it also captures on-disk CME signatures in a physically self-consistent manner.…”

Section: Introductionmentioning

confidence: 94%

Three‐dimensional and twisted: An MHD interpretation of on‐disk observational characteristics of coronal mass ejections

Gibson¹,

Low²

2000

J. Geophys. Res.

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Abstract. A physical interpretation of observed coronal "on-disk" manifestations of an Earth-directed coronal mass ejection (CME) is presented. The fundamental question of how the CME's magnetic field and its plasma distribution are related is largely unanswered, because a crucial piece of the puzzle, that is the threedimensional (3-D) morphology of the CME, remains diflScult to ascertain so long as coronal observations are limited to projections onto a single plane of the sky. In order •o understand the relationship between observations of CMEs projected at the solar limb and those projected on the solar disk, some sort of model of the 3-D CME is required. In this paper we address both the question of the 3-D morphology of the CME and the more fundamental question of the nature of the plasma-magnetic field relationship, by comparing the limb and on-disk CME representations of an analytic 3-D MHD model based on a spheromak-type flux rope magnetic field configuration. In particular, we show that the morphology of twin dimmings (also referred to as transient coronal holes) observed in X ray and EUV can be reproduced by the CME model as the on-disk prbjection of the prominence cavity modeled for limb CMEs. Moreover, the bright core of a limb CME, generally corresponding to the material in an erupting prominence, may be interpreted to be the S-shaped central core of the modeled on-disk CME, splitting the cavity into twin dimmings when observed head-on without obstruction. The magnetic field structure of this central core exhibits many of a filament's magnetic field features required to match observations. Finally, we consider the nature of S-shaped filaments and X-ray "sigmoids" in the context of the model, in terms of localized heating and cooling acting on the modeled CME magnetic field structure.

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Section: Introductionmentioning

confidence: 94%

Three‐dimensional and twisted: An MHD interpretation of on‐disk observational characteristics of coronal mass ejections

Gibson¹,

Low²

2000

J. Geophys. Res.

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“…This flux rope is either developed as part of the supporting structure necessary for the initial development of the solar prominence or as a result of field lines reconnecting during the eruption. Aside from the spacecraft observations, the flux rope configuration also explains the white-light structure of CMEs (Chen 1996;Gibson & Low 1998. Gibson et al (2006) reported a more recent, comprehensive survey of white-light quiescent cavities (associated with a range of coronal loop morphologies) that suggested that the flux rope structure is formed prior to initiation of the CME.…”

Section: Flux Rope Modeling Of Cmesmentioning

confidence: 99%

VLA Measurements of Faraday Rotation through Coronal Mass Ejections

et al. 2017

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Coronal mass ejections (CMEs) are large-scale eruptions of plasma from the Sun that play an important role in space weather. Faraday rotation (FR) is the rotation of the plane of polarization that results when a linearly polarized signal passes through a magnetized plasma such as a CME and is proportional to the path integral through the plasma of the electron density and the line of sight component of the magnetic field.FR observations of a source near the Sun can provide information on the plasma structure of a CME shortly after launch; however, separating the contribution of the plasma density from the line of sight magnetic field is challenging.We report on simultaneous white-light and radio observations made of three CMEs in August 2012. We made sensitive Very Large Array (VLA) full-polarization observations using 1 − 2 GHz frequencies of a "constellation" of radio sources through the solar corona at heliocentric distances that ranged from 6 − 15R ⊙ . Of the nine sources observed, three were occulted by CMEs: two sources (0842+1835 and 0900+1832) were occulted by a single CME and one source (0843+1547) was occulted by two CMEs. In addition to our radioastronomical observations, which represent one of the first active hunts for CME Faraday rotation since Bird et al. (2007) and Jensen & Russell (2008), as well as previous CME FR observations by Bird et al. (1985).

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“…In this study, we initiate CMEs using the analytical GL (Gibson & Low 1998) flux rope model implemented in the Eruptive Event Generator Gibson Low module. This flux rope model has been successfully used in numerous studies modeling CMEs (e.g., Manchester et al 2004aManchester et al , 2004bManchester et al , 2014Lugaz et al 2005aLugaz et al , 2005bSchmidt & Ofman 2010).…”

Section: Gl Flux Rope Modelmentioning

confidence: 99%

A Numerical Study of Long-Range Magnetic Impacts During Coronal Mass Ejections

Jin

Schrijver

Cheung

et al. 2016

ApJ

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With the global view and high-cadence observations from Solar Dynamics Observatory/Atmospheric Imaging Assembly and Solar TErrestrial RElations Observatory, many spatially separated solar eruptive events appear to be coupled. However, the mechanisms for "sympathetic" events are still largely unknown. In this study, we investigate the impact of an erupting flux rope on surrounding solar structures through large-scale magnetic coupling. We build a realistic environment of the solar corona on 2011 February 15 using a global magnetohydrodynamics model and initiate coronal mass ejections (CMEs) in active region 11158 by inserting Gibson-Low analytical flux ropes. We show that a CME's impact on the surrounding structures depends not only on the magnetic strength of these structures and their distance to the source region, but also on the interaction between the CME and the large-scale magnetic field. Within the CME expansion domain where the flux rope field directly interacts with the solar structures, expansion-induced reconnection often modifies the overlying field, thereby increasing the decay index. This effect may provide a primary coupling mechanism underlying the sympathetic eruptions. The magnitude of the impact is found to depend on the orientation of the erupting flux rope, with the largest impacts occurring when the flux rope is favorably oriented for reconnecting with the surrounding regions. Outside the CME expansion domain, the influence of the CME is mainly through field line compression or post-eruption relaxation. Based on our numerical experiments, we discuss a way to quantify the eruption impact, which could be useful for forecasting purposes.

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A Time‐dependent Three‐dimensional Magnetohydrodynamic Model of the Coronal Mass Ejection

Cited by 300 publications

References 44 publications

Three‐dimensional and twisted: An MHD interpretation of on‐disk observational characteristics of coronal mass ejections

Three‐dimensional and twisted: An MHD interpretation of on‐disk observational characteristics of coronal mass ejections

VLA Measurements of Faraday Rotation through Coronal Mass Ejections

A Numerical Study of Long-Range Magnetic Impacts During Coronal Mass Ejections

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