A Numerical Study of the Breakout Model for Coronal Mass Ejection Initiation

MacNeice, P. J.; Antiochos, S. K.; Phillips, Andrew Duncan; Spicer, D. S.; DeVore, C. R.; Olson, K.

doi:10.1086/423887

Cited by 133 publications

(108 citation statements)

References 48 publications

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“…This dynamical process is the same as the breakout CME scenario. However, the inclusion of a background wind and helmet streamer makes the further evolution of the breakout CME different from the more idealised simulations of Antiochos et al (1999); MacNeice et al (2005). Figure 4c shows a more complex topology including two flux ropes.…”

Section: Topological Evolutionmentioning

confidence: 95%

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Modelling the initiation of coronal mass ejections: magnetic flux emergence versus shearing motions

Zuccarello¹,

Jacobs²,

Soenen³

et al. 2009

A&A

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Context. Coronal mass ejections (CMEs) are enormous expulsions of magnetic flux and plasma from the solar corona into the interplanetary space. These phenomena release a huge amount of energy. It is generally accepted that both photospheric motions and the emergence of new magnetic flux from below the photosphere can put stress on the system and eventually cause a loss of equilibrium resulting in an eruption. Aims. By means of numerical simulations we investigate both emergence of magnetic flux and shearing motions along the magnetic inversion line as possible driver mechanisms for CMEs. The pre-eruptive region consists of three arcades with alternating magnetic flux polarity, favouring the breakout mechanism.Methods. The equations of ideal magnetohydrodynamics (MHD) were advanced in time by using a finite volume approach and solved in spherical geometry. The simulation domain covers a meridional plane and reaches from the lower solar corona up to 30 R . When we applied time-dependent boundary conditions at the inner boundary, the central arcade of the multiflux system expands, leading to the eventual eruption of the top of the helmet streamer. We compare the topological and dynamical evolution of the system when driven by the different boundary conditions. The available free magnetic energy and the possible role of magnetic helicity in the onset of the CME are investigated. Results. In our simulation setup, both driving mechanisms result in a slow CME. Independent of the driving mechanism, the overall evolution of the system is the same: the actual CME is the detatched helmet streamer. However, the evolution of the central arcade is different in the two cases. The central arcade eventually becomes a flux rope in the shearing case, whereas in the flux emergence case there is no formation of a flux rope. Furthermore, we conclude that magnetic helicity is not crucial to a solar eruption.

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Section: Topological Evolutionmentioning

confidence: 95%

“…The reconnection site is located above the central arcade that reconnects with the overlying field to create a passage for the CME. Subsequently, MacNeice et al (2005) used more sophisticated numerical techniques to investigate the behaviour of CMEs in a breakout scenario and show that fast CMEs can be produced.…”

Section: Introductionmentioning

confidence: 99%

Modelling the initiation of coronal mass ejections: magnetic flux emergence versus shearing motions

Zuccarello¹,

Jacobs²,

Soenen³

et al. 2009

A&A

View full text Add to dashboard Cite

show abstract

“…Antiochos 1998;Antiochos et al 1999;MacNeice et al 2004;Lynch et al 2004;Choe et al 2005). The equilibrium set-up of the magnetic breakout model model consists of a quadrupolar photospheric flux distribution coupled with an overlying field, and such a set-up contains a coronal null point.…”

Section: Statistics Of Coronal Null Pointsmentioning

confidence: 99%

Review Article: MHD Wave Propagation Near Coronal Null Points of Magnetic Fields

McLaughlin¹,

Hood²,

Moortel³

2010

Space Sci Rev

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We present a comprehensive review of MHD wave behaviour in the neighbourhood of coronal null points: locations where the magnetic field, and hence the local Alfvén speed, is zero. The behaviour of all three MHD wave modes, i.e. the Alfvén wave and the fast and slow magnetoacoustic waves, has been investigated in the neighbourhood of 2D, 2.5D and (to a certain extent) 3D magnetic null points, for a variety of assumptions, configurations and geometries. In general, it is found that the fast magnetoacoustic wave behaviour is dictated by the Alfvén-speed profile. In a β = 0 plasma, the fast wave is focused towards the null point by a refraction effect and all the wave energy, and thus current density, accumulates close to the null point. Thus, null points will be locations for preferential heating by fast waves. Independently, the Alfvén wave is found to propagate along magnetic fieldlines and is confined to the fieldlines it is generated on. As the wave approaches the null point, it spreads out due to the diverging fieldlines. Eventually, the Alfvén wave accumulates along the separatrices (in 2D) or along the spine or fan-plane (in 3D). Hence, Alfvén wave energy will be preferentially dissipated at these locations. It is clear that the magnetic field plays a fundamental role in the propagation and properties of MHD waves in the neighbourhood of coronal null points. This topic is a fundamental plasma process and results so far have also lead to critical insights into reconnection, mode-coupling, quasi-periodic pulsations and phase-mixing.

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“…Amari et al (2000) investigated, in a simple bipolar topology, the role of flux cancellation in the destabilization of a flux rope formed by shearing/twisting motions and later studied it in a complex multiflux configuration (Amari et al 2007). An alternative model is the breakout scenario (Antiochos et al 1999;MacNeice et al 2005), where the vulnerability of multipolar topologies to rearrangements of the magnetic field's connectivity is exploited to enable the eruption. Here, the reconnection site is located above the sheared arcade which reconnects with the overlying field to create a passage for the CME.…”

Section: Introductionmentioning

confidence: 99%

Numerical simulations of homologous coronal mass ejections in the solar wind

Soenen¹,

Zuccarello²,

Jacobs³

et al. 2009

A&A

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Context. Coronal mass ejections (CMEs) are enormous expulsions of magnetic flux and plasma from the solar corona. Most scientists agree that a coronal mass ejection is the sudden release of magnetic free energy stored in a strongly stressed field. However, the exact reason for this sudden release is still highly debated. Aims. In an initial multiflux system in steady state equilibrium, containing a pre-eruptive region consisting of three arcades with alternating magnetic flux polarity, we study the initiation and early evolution properties of a sequence of CMEs by shearing a region slightly larger than the central arcade. Methods. We solve the ideal magnetohydrodynamics (MHD) equations in an axisymmetrical domain from the solar surface up to 30 R . The ideal MHD equations are advanced in time over a non uniform grid using a modified version of the Versatile Advection Code (VAC). Results. By applying shearing motions on the solar surface, the magnetic field is energised and multiple eruptions are obtained. Magnetic reconnection first opens the overlying field and two new reconnections sites set in on either side of the central arcade. After the disconnection of the large helmet top, the system starts to restore itself but cannot return to its original configuration as a new arcade has already started to erupt. This process then repeats itself as we continue shearing. Conclusions. The simulations reported in the present paper, demonstrate the ability to obtain a sequence of CMEs by shearing a large region of the central arcade or by shearing a region that is only slightly larger than the central arcade. We show, be it in an axisymmetric configuration, that the breakout model can not only lead to confined eruptions but also to actual coronal mass ejections provided the model includes a realistic solar wind model.

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A Numerical Study of the Breakout Model for Coronal Mass Ejection Initiation

Cited by 133 publications

References 48 publications

Modelling the initiation of coronal mass ejections: magnetic flux emergence versus shearing motions

Modelling the initiation of coronal mass ejections: magnetic flux emergence versus shearing motions

Review Article: MHD Wave Propagation Near Coronal Null Points of Magnetic Fields

Numerical simulations of homologous coronal mass ejections in the solar wind

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