3-D nonlinear evolution of MHD instabilities

Bateman, G.; Hicks, H.R.; Wooten, J.W.; Dory, R.A.

doi:10.2172/7222828

Cited by 161 publications

(246 citation statements)

References 2 publications

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“…Another possibility, however, is that the newly formed rope becomes subject to an ideal MHD instability. A likely candidate is the torus instability (Bateman 1978;Kliem & Török 2006;Török & Kliem 2007). A toroidal flux tube will become unstable against expansion if the external poloidal field decreases sufficiently rapidly in the direction of the major tube radius.…”

Section: Resultsmentioning

confidence: 99%

Multiple eruptions from magnetic flux emergence

MacTaggart

Hood

2009

A&A

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Aims. In this paper we study the effects of a toroidal magnetic flux tube emerging into a magnetized corona, with an emphasis on large-scale eruptions. The orientation of the fields is such that the two flux systems are almost antiparallel when they meet. Methods. We follow the dynamic evolution of the system by solving the 3D MHD equations using a Lagrangian remap scheme. Results. Multiple eruptions are found to occur. The physics of the trigger mechanisms is discussed and related to well-known eruption models.

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Section: Resultsmentioning

confidence: 99%

Multiple eruptions from magnetic flux emergence

MacTaggart

Hood

2009

A&A

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“…Bateman 1980; for an analysis in the context of sunspots see Meyer et al 1977). This is the case with the boundaries of the pores seen in Fig.…”

Section: Flutingmentioning

confidence: 88%

Striation and convection in penumbral filaments

Spruit¹,

Scharmer

Löfdahl

2010

A&A

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Observations with the 1-m Swedish Solar Telescope of the flows seen in penumbral filaments are presented. Time sequences of bright filaments show overturning motions strikingly similar to those seen along the walls of small isolated structures in the active regions. The filaments show outward propagating striations with inclination angles suggesting that they are aligned with the local magnetic field. We interpret it as the equivalent of the striations seen in the walls of small isolated magnetic structures. Their origin is then a corrugation of the boundary between an overturning convective flow inside the filament and the magnetic field wrapping around it. The outward propagation is a combination of a pattern motion due to the downflow observed along the sides of bright filaments, and the Evershed flow. The observed short wavelength of the striation argues against the existence of a dynamically significant horizontal field inside the bright filaments. Its intensity contrast is explained by the same physical effect that causes the dark cores of filaments, light bridges and "canals". In this way striation represents an important clue to the physics of penumbral structure and its relation with other magnetic structures on the solar surface. We put this in perspective with results from the recent 3-D radiative hydrodynamic simulations.

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“…There is little doubt that filaments are enclosed within flux ropes. We can estimate the stability of flux rope equilibrium in the coronal magnetic field knowing its height above the photosphere and calculating the so-called decay index n (Bateman 1978;Filippov & Den 2000, 2001Kliem & Török 2006;Démoulin & Aulanier 2010;Zuccarello et al 2014). The stable equilibrium is possible only if the background field decreases with height not too fast, or the decay index of the ambient magnetic field does not exceed a critical value nc.…”

Section: Discussionmentioning

confidence: 99%

Formation of a rotating jet during the filament eruption on 2013 April 10–11

Filippov

Srivastava

Dwivedi

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We analyze multi-wavelength and multi-viewpoint observations of a helically twisted plasma jet formed during a confined filament eruption on 10-11 April 2013. Given a rather large scale event with its high spatial and temporal resolution observations, it allows us to clearly understand some new physical details about the formation and triggering mechanism of twisting jet. We identify a pre-existing flux rope associated with a sinistral filament, which was observed several days before the event. The confined eruption of the filament within a null point topology, also known as an Eiffel tower (or inverted-Y) magnetic field configuration results in the formation of a twisted jet after the magnetic reconnection near a null point. The sign of helicity in the jet is found to be the same as that of the sign of helicity in the filament. Untwisting motion of the reconnected magnetic field lines gives rise to the accelerating plasma along the jet axis. The event clearly shows the twist injection from the pre-eruptive magnetic field to the jet.

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3-D nonlinear evolution of MHD instabilities

Cited by 161 publications

References 2 publications

Multiple eruptions from magnetic flux emergence

Multiple eruptions from magnetic flux emergence

Striation and convection in penumbral filaments

Formation of a rotating jet during the filament eruption on 2013 April 10–11

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