LARGE-SCALE HYDRODYNAMIC FLOWS IN MEDIA WITH VARIABLE THERMODYNAMIC CHARACTERISTICS

Мұқаба

Дәйексөз келтіру

Толық мәтін

Аннотация

A theory of large-scale flows in a rotating astrophysical plasma under conditions of non-trivial properties of the physical medium, which are not described by the classical hydrodynamic theory of plasma, is developed. As a first step, the theory is developed within a neutral fluid model to describe astrophysical plasma, with a subsequent generalization in mind to take into account magnetic effects. Such a model is of independent importance for studying turbulent dynamo in star-forming regions in galaxies and hydrodynamic instabilities in poorly ionized disks, for describing meridional flows below convective zones in lowmass stars and on the Sun, aswell as for studying oscillations of the Sun and stars. Therefore, the results obtained have a wider application, e.g., for describing geophysical currents. The theory is based on two key ideas developed in plasma astrophysics: the use of a shallow water model with large-scale compressibility and the use of a two-layer shallow water model. Equations for two-layer shallow water are derived taking into account rotation and the effect of flow sphericity on rotation, in which the effects of large-scale compressibility are taken into account in the upper layer. For a rotating system, dispersion relations are obtained for Poincar. waves in two-layer shallow water, taking into account large-scale compressibility; similar dispersion relations for Poincar. waves are obtained in the high-frequency limit taking into account the effect of sphericity on rotation; in the low-frequency limit, a dispersion relation is obtained for Rossby waves. It is shown that the dispersion relations for Poincar. waves, taking into account the sphericity of the flow, have a qualitatively different form, which leads to three-wave interactions of Poincar. waves and the interaction of two Poincar. waves with a Rossby wave, which are not observed in a single-layer flow of a compressible fluid. All types of three-wave interactions for the flows under consideration are studied using the method of multiscale expansions.

Авторлар туралы

M. Yudenkova

Space Research Institute, Russian Academy of Sciences; Moscow Institute of Physics and Technology (State University)

Moscow, Russia; Dolgoprudnyi, Russia

D. Klimachkov

Space Research Institute, Russian Academy of Sciences

Moscow, Russia

A. Petrosyan

Space Research Institute, Russian Academy of Sciences; Moscow Institute of Physics and Technology (State University)

Email: apetrosy@iki.rssi.ru
Moscow, Russia; Dolgoprudnyi, Russia

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