Two-dimensional magnetohydrodynamic model of emerging magnetic flux in the solar atmosphere

Shibata, Kazunari; Tajima, T.; Steinolfson, R. S.; Matsumoto, Ryoji

doi:10.1086/167932

Cited by 143 publications

(112 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Shibata et al 1989;Fan 2001;Archontis et al 2004). It has been shown that the flux tube rises due to the Parker instability (Parker 1966) and expands into the corona in a self-similar way, which explains the characteristics of the flux emergence such as Ω-shaped loops and the downflows at the footpoints of the loops.…”

Section: Introductionmentioning

confidence: 95%

Large-scale 3D MHD simulation on the solar flux emergence and the small-scale dynamic features in an active region

Toriumi

Yokoyama

2012

A&A

View full text Add to dashboard Cite

We have performed a three-dimensional magnetohydrodynamic simulation to study the emergence of a twisted magnetic flux tube from −20 000 km of the solar convection zone to the corona through the photosphere and the chromosphere. The middle part of the initial tube is endowed with a density deficit to instigate a buoyant emergence. As the tube approaches the surface, it extends horizontally and makes a flat magnetic structure due to the photosphere ahead of the tube. Further emergence to the corona breaks out via the interchange-mode instability of the photospheric fields, and eventually several magnetic domes build up above the surface. What is new in this three-dimensional experiment is multiple separation events of the vertical magnetic elements are observed in the photospheric magnetogram, and they reflect the interchange instability. Separated elements are found to gather at the edges of the active region. These gathered elements then show shearing motions. These characteristics are highly reminiscent of active region observations. On the basis of the simulation results above, we propose a theoretical picture of the flux emergence and the formation of an active region that explains the observational features, such as multiple separations of faculae and the shearing motion.

show abstract

Section: Introductionmentioning

confidence: 95%

Large-scale 3D MHD simulation on the solar flux emergence and the small-scale dynamic features in an active region

Toriumi

Yokoyama

2012

A&A

View full text Add to dashboard Cite

show abstract

“…Much of the pioneering work on simulating flux emergence was started by Shibata and co-workers , 1990, Shibata, Nozawa, and Matsumoto, 1992, Yokoyama and Shibata, 1995. While this work was mainly 2D, it laid the foundations for the subsequent 3D simulations.…”

Section: Introductionmentioning

confidence: 99%

3D MHD Flux Emergence Experiments: Idealised Models and Coronal Interactions

Hood

Archontis

MacTaggart³

2011

Sol Phys

View full text Add to dashboard Cite

This paper reviews some of the many 3D numerical experiments of the emergence of magnetic fields from the solar interior and the subsequent interaction with the pre-existing coronal magnetic field. The models described here are idealized, in the sense that the internal energy equation only involves the adiabatic, Ohmic and viscous shock heating terms. However, provided the main aim is to investigate the dynamical evolution, this is adequate. Many interesting observational phenomena are explained by these models in a self-consistent manner.

show abstract

“…Numerical experiments to simulate the emergence process started with the pioneering 2D work of Shibata et al (1989), Shibata et al (1992) who studied the emergence in a highly stratified atmosphere of a horizontal flux sheet through the development of a buoyancy instability and found a self-similar behaviour in the nonlinear phase of the evolution. Further developments of this work were reported by and Nozawa et al (1992).…”

Section: Introductionmentioning

confidence: 99%

The emergence of toroidal flux tubes from beneath the solar photosphere

Hood¹,

Archontis²,

Galsgaard³

et al. 2009

A&A

View full text Add to dashboard Cite

Context. Models of flux emergence frequently use a twisted cylindrical loop as the initial starting configuration and ignore the coupling between the radiation field and plasma. In these models, the axis of the original tube never emerges through the photosphere. Without the axis emerging, it is very difficult to form a realistic sunspot. Aims. The aim is to use a toroidal flux loop, placed beneath the solar photosphere and study whether the axis of the system emerges fully into the atmosphere. The toroidal curvature means that the plasma can drain more effectively than in a straight cylindrical tube. Methods. Three-dimensional magnetohydrodynamic numerical simulations of an emerging magnetic flux tube are presented for an initial toroidal loop model. The simulations use a Lagrangian-Remap code that is particularly suited to dealing with shocks and strong current sheets. Results. The evolution of the toroidal loop is followed and the characteristics of the emergence process are compared with the traditional cylindrical loops. The flux sources seen at the photosphere are more circular, and there are less shearing motions in the upper photosphere. When the initial magnetic field strength is relatively weak the evolution of the system is similar to the cylindrical loop case, with the formation of a new flux rope above the photosphere. A striking result is that for large values of field strength the axial field of the toroidal loop emerges fully into the corona. This is reported for the first time in experiments of flux emergence in a highly stratified atmosphere that do not solve self-consistently the radiation transfer problem. In addition, the new flux rope forms below the original axis of the toroidal tube when the field strength is sufficiently strong.

show abstract

Two-dimensional magnetohydrodynamic model of emerging magnetic flux in the solar atmosphere

Cited by 143 publications

References 0 publications

Large-scale 3D MHD simulation on the solar flux emergence and the small-scale dynamic features in an active region

Large-scale 3D MHD simulation on the solar flux emergence and the small-scale dynamic features in an active region

3D MHD Flux Emergence Experiments: Idealised Models and Coronal Interactions

The emergence of toroidal flux tubes from beneath the solar photosphere

Contact Info

Product

Resources

About