Results 191 to 200 of about 2,286 (221)

Stability of solar coronal loops

Computer Physics Communications, 1990
Abstract The equations of magnetohydrodynamics do not contain an intrinsic length scale determining the size of phenomena. Hence, size only enters through the external geometrical properties of the configurations considered. This is one of the reasons why tokamaks and solar coronal loops may be considered as similar objects.
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Solar and stellar coronal loops

Advances in Space Research, 1991
Abstract X-ray and EUV pictures from space experiments (e.g. SKYLAB ) have revealed that the corona of the Sun consists of a variety of discrete structures - involving a range of timescales - which appear to outline the magnetic field lines emerging from the convection zone below the photosphere.
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Magnetic reconnection in solar coronal loops

Advances in Space Research, 1997
Abstract Simulations of the evolution of kink modes in line-tied coronal loops are presented which demonstrate the occurrence of magnetic reconnection in the non-linear stage of the instability. In loops which do not carry a net axial current (and are confined by a potential purely axial field) the reconnection is limited to the initial current ...
G Einaudi, R Lionello, M Velli
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Temporal evolution of resonant absorption in solar coronal loops

Computer Physics Communications, 1990
Abstract A numerical code is presented for the computation of the temporal evolution of an externally driven cylindrical plasma column in the framework of linearized compressible and resistive magnetohydrodynamics. The partial differential equations are solved with a semi-discretization method using cubic and quadratic finite elements for the spatial
Poedts, S., Goossens, M., Kerner, W.
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Intermittent heating in a model of solar coronal loops

Solar Physics, 2000
X-ray and EUV observations of the solar corona reveal a very complex and dynamic environment where there are many examples of structures that are believed to outline the Sun's magnetic field. In this present study, the authors investigate the temporal response of the temperature, density and pressure of a solar coronal plasma contained within a ...
R.W. Walsh, S. Galtier
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Nonlinear wave heating of solar coronal loops.

Astronomy and Astrophysics, 1997
The heating of magnetically closed structures (loops) in the solar corona by the resonant absorption of incident waves is studied by means of numerical simulations in the framework of nonlinear resistive magnetohydrodynamics (MHD). It is shown that the dynamics in the resonant layer is indeed very nonlinear for typical coronal parameters. The effect of
Poedts, S., Goedbloed, J.P.
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Temporal behaviour of pressure in solar coronal loops

Solar Physics, 1995
The temporal evolution of pressure in solar coronal loops is studied using the ideal theory of magnetohydrodynamic turbulence in cylindrical geometry. The velocity and the magnetic fields are expanded in terms of the Chandrasekhar-Kendall (C-K) functions. The three-mode representation of the velocity and the magnetic fields submits to the investigation
K. Sasidharan, T. D. Sreedharan, R. Pratap, V. Krishan   +3 more
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Pressure structure of solar coronal loops, III

Solar Physics, 1992
The theory of ideal magnetohydrodynamic turbulence in cylindrical geometry is used to study the steady-state structure of a coronal loop. The pressure profile is derived from MHD equations by representing the velocity and magnetic fields as the superposition of Chandrasekhar-Kendall functions.
T. D. Sreedharan, K. Sasidharan, A. Satya Narayanan, V. Krishan   +3 more
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Explosive Instability in Solar Coronal Loops

1991
The presence of shear flows along the stretched magnetic field structures such as solar coronal loops change their dynamics essentially, and, particularly, can lead to the explosive instabilty which results in the fast and efficient energy release.
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A Model for Intermediate Temperature Solar Coronal Loops

Publications of the Astronomical Society of Australia, 1992
AbstractSimple hydrostatic equilibrium models have been very successful at describing the physical conditions in hot coronal loops (T > 106 K). However, equilibrium models of cooler loops predict densities that are much lower than observed. We follow the evolution of a hot loop which undergoes a sudden reduction in heat input.
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