Stability analysis of two-dimensional models of quiescent prominences

Trejo, Jesús Galindo

doi:10.1007/bf00214166

Cited by 15 publications

(8 citation statements)

References 28 publications

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“…Lerche and Low (1980) model. These panels do not include all configurations inspected by Galindo Trejo (1987) The spatial distribution of motions is similar to that found by Galindo Trejo (1987) for Menzel's and Lerche and Low's equilibrium models.…”

Section: Stability Of Two-dimensional Prominence Modelsmentioning

confidence: 60%

“…Some two-dimensional equilibrium models were considered by Galindo Trejo (1987Trejo ( , 1989bTrejo ( , a, 1998Trejo ( , 2006. The focus of these works was in the stability properties of prominence equilibrium configurations (using the MHD energy principle of Bernstein et al 1958) and for this reason the author concentrated in the lowest eigenvalue squared.…”

Section: Stability Of Two-dimensional Prominence Modelsmentioning

confidence: 99%

“…Galindo Trejo (1987) considered four prominence models, namely those by Kippenhahn and Schlüter (1957), Dungey (1953), Menzel (1951) and Lerche and Low (1980). All these models are isothermal, i.e., they do not incorporate the corona around the prominence plasma.…”

Section: Stability Of Two-dimensional Prominence Modelsmentioning

confidence: 99%

“…This implies that the important hybrid modes are absent in the analysis. In spite of this, some interesting results were obtained by Galindo Trejo (1987). Here we only mention the most relevant ones.…”

Section: Stability Of Two-dimensional Prominence Modelsmentioning

confidence: 99%

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Prominence oscillations

Arregui

Oliver

Ballester

2018

Living Rev Sol Phys

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Prominences are intriguing, but poorly understood, magnetic structures of the solar corona. The dynamics of solar prominences has been the subject of a large number of studies, and of particular interest is the study of prominence oscillations. Ground-and space-based observations have confirmed the presence of oscillatory motions in prominences and they have been interpreted in terms of magnetohydrodynamic waves. This interpretation opens the door to perform prominence seismology, whose main aim is to determine physical parameters in magnetic and plasma structures (prominences) that are difficult to measure by direct means. Here, we review the This article is a revised version of https://doi.org/10.12942/lrsp-2012-2. Change summary: Major revision, updated and expanded. Change details: New section on Bayesian analysis. New observations and theoretical models for small and for large amplitude oscillations. About 50 new references were added.

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Section: Stability Of Two-dimensional Prominence Modelsmentioning

confidence: 60%

Section: Stability Of Two-dimensional Prominence Modelsmentioning

confidence: 99%

Section: Stability Of Two-dimensional Prominence Modelsmentioning

confidence: 99%

Section: Stability Of Two-dimensional Prominence Modelsmentioning

confidence: 99%

See 2 more Smart Citations

Prominence oscillations

Arregui

Oliver

Ballester

2018

Living Rev Sol Phys

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“…In the first class (e.g., Anzer 1969;Wu 1987;Aly et al 1994;Lepeltier & Aly 1996), the prominence is modeled as an infinitely thin sheet of plasma which is maintained in equilibrium against the solar gravitational field by an upward-directed magnetic tension force exerted by an external potential field having its lines firmly anchored in a rigid boundary representing the dense photosphere. In the second class (e.g., Zweibel 1981Zweibel , 1982Galindo-Trejo & Schindler 1984;Galindo Trejo 1987), the plasma is taken to be distributed in a continuous way in the dips of a magnetic "hammocklike" structure. In the latter context, Zweibel (1982) has shown that a 2D equilibrium with a uniform total (thermal+magnetic) pressure-like the standard Kippenhahn-Schlüter equilibrium (KSEq; Kippenhahn & Schlüter 1957)-is linearly stable, and a similar result has been reported by Galindo-Trejo & Schindler (1984).…”

Section: Introductionmentioning

confidence: 99%

Nonlinear Stability of a Class of Magnetostatic Equilibria With an Application to Solar Prominences

Aly¹

2012

ApJ

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We consider a particular class of three-dimensional magnetostatic equilibria in which the plasma is submitted to a vertical gravitational field and the gradient of the total (thermal+magnetic) pressure vanishes. We show analytically that an equilibrium in that class makes the energy an absolute minimum in the set of all the configurations accessible from it by an arbitrary finite deformation constrained by ideal MHD and imposed to vanish on a rigid conducting wall (line-tying condition). Along with energy conservation, this implies the nonlinear ideal stability of that equilibrium in the following sense. Suppose that a perturbation of energy w(0) is applied at time t = 0 and thus evolves by obeying the nonlinear MHD equations. Then some measure of the sizes of the plasma velocity and the deformation of the structure can be made to stay at any t 0 below an arbitrarily prescribed value by choosing w(0) small enough. Nonlinear stability also holds true for a configuration obtained by superposing an equilibrium of the previous type and a nonmagnetic equilibrium which is also an energy minimizer-for instance an equilibrium with uniform specific entropy, which is shown to have that property. Our result applies to a subset of a family of equilibria, computed by B. C. Low, which includes in particular the standard Kippenhahn-Schlüter model describing the magnetic support of solar corona prominences.

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Hydromagnetic stability analysis of a Solar prominence suspended in an external horizontal magnetic field

Galindo-Trejo¹

1998

Astron Nachr

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Among the observed characteristics of quiescent solar prominences, stability is perhaps the most important requirement for theoretical models of these coronal structures. Only stable equilibria can explain the presence of such cool and dense plasma sheets for extended periods of time. Utilizing the MHD-Energy Principle (Bernstein et al. 1958) we investigate the linear stability properties of the two-dimensional prominence equilibrium of Osherovich (1985). Incorporating a finite magnetic energy and a continous magnetic field, this model takes into account explicitly an external horizontal magnetic field in which the prominence is suspended. The presented numerical calculations indicate that the prominence model of Osherovich is stable and can explain the main features of reported oscillations. Instabilities occur only when model parameters are unrealistic for physical conditions in solar prominences.

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Stability analysis of two-dimensional models of quiescent prominences

Cited by 15 publications

References 28 publications

Prominence oscillations

Prominence oscillations

Nonlinear Stability of a Class of Magnetostatic Equilibria With an Application to Solar Prominences

Hydromagnetic stability analysis of a Solar prominence suspended in an external horizontal magnetic field

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