The Effect of Spirality on the Evolution of Turbulence in the Solar Protoplanetary Cloud
We use the methods of nonequilibrium thermodynamics to prove the possibility of the development of negative viscosity in the three-dimensional case in terms of the twoscale hydrodynamic description of maximally developed disk turbulence. Negative viscosity in a rotating disk system appears to be a manifestation of cascade processes in spiral turbulence where inverse energy transfer from small to larger vortices occurs. Within the framework of asymmetric mechanics of turbulized continua, we physically substantiated the phenomenological formula for the turbulent stress tensor of Wasiutynski, which is widely used in the astrophysical literature to explain the differential rotation of various cosmic objects by “anisotropic viscosity.” The aim of our study is, first and foremost, to improve a number of representative hydrodynamic models of cosmic natural turbulized media, including the birth of galaxies and galaxy clusters, birth of stars from the diffuse medium of gas and dust clouds, formation of accretion disks and subsequent accumulation of planetary systems, and also the formation of gaseous envelopes of planets, atmospheres, etc. This paper continues the application of stochastic and thermodynamic approach to the synergetic description of the structured turbulence of astrogeophysical systems, which we have been developing in a series of our papers
(Kolesnichenko, 2004, 2005; Kolesnichenko and Marov, 2006; Marov and Kolesnichenko, 2002, 2006).
Mathematical modelling in actual problems of science and technics