Study of vortex breakdown in a stratified fluid

Кшевецкий, С. П.

doi:10.1134/s0965542506110133

Cited by 4 publications

(2 citation statements)

References 18 publications

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“…This makes it possible to describe small-scale turbulence and discontinuities, automatically passing, whenever necessary, to the use of the class of generalised functions. This technique was verified in our previous studies (Kshevetskii and Gavrilov, 2005;Kshevetskii, 2006;Kshevetskii, 2006, 2011)). This allows us to obtain solutions for comparatively long time intervals even if small-scale perturbations develop.…”

Section: Introductionsupporting

confidence: 76%

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Numerical MHD Simulation of the Coupled Evolution of Plasma and Magnetic Field in the Solar Chromosphere. I. Gradual and Impulsive Energisation

Alekseeva

Кшевецкий

2015

Sol Phys

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The dynamical coupling between the solar chromospheric plasma and magnetic field is investigated by numerically solving a fully self-consistent, twodimensional initial-value problem for the nonlinear collisional MHD equations including electric resistivity, thermal conduction, and, in some cases, gas-dynamic viscosity. The processes in the contact zone between two horizontal magnetic fields of opposite polarities are considered. The plasma is assumed to be initially motionless and having a temperature of 50,000 K uniform throughout the plasma volume; the characteristic magnetic field corresponds to a plasma β 1. In a physical-time interval of 17 seconds typically covered by a computational run, the plasma temperature gradually increases by a factor of two to three. Against this background, an impulsive (in 0.1 seconds or less) increase in the current-aligned plasma velocity occurs at the site of the current-layer thinning (sausage-type deformation, or m = 0 pinch instability). Such a "velocity burst" can be interpreted physically as an event of suprathemal-proton generation. Further development of the sausage instability results in an increase in the kinetic temperature of the protons to high values, even to those observed in flares. The form of our system of MHD equations indicates that such increases are a property of the exact solution of the system at an appropriate choice of the parameters. Magnetic reconnection does not manifest itself in this solution: it would generate flows forbidden by the chosen geometry. Therefore, the pinch-sausage effect can act as an energiser of the upper chromosphere and be an alternative to the magnetic-reconnection process as the producer of flares.

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Section: Introductionsupporting

confidence: 76%

“…Structurally, the numerical-integration formulas resemble those of the Lax-Wendroff method. A comprehensive analysis of our numerical technique was given by Kshevetskii (2006).…”

Section: The Procedures Of Numerical Solutionmentioning

confidence: 99%