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 Matem. Mod., 2008, Volume 20, Number 10, Pages 99–125 (Mi mm2581)

Role of hydrodynamic helicity in evolution of the protoplanetary turbulent disc

A. V. Kolesnichenko, M. Ya. Marov

M. V. Keldysh Institute for Applied Mathematics, Russian Academy of Sciences

Abstract: We analyze the possible effect of hydrodynamic spirality that develops in a rotating disk on the synergetic structurization of cosmic matter and on the development of negative turbulent viscosity in cosmic matter within the framework of the problem of the reconstruction of the evolution of the protoplanetary cloud that surrounded the early Sun. We show that comparatively slow damping of turbulence in the disk can be partially due to the lack of reflective symmetry of the anisotropic field of turbulent velocities about its equatorial plane. We formulate the general concept of the development of energy-intensive coherent mesoscale vortex structures in the thermodynamically open system of turbulent chaos associated with the realization of inverse cascade of kinetic energy in mirror?nonsymmetrical disk turbulence. 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.

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Citation: A. V. Kolesnichenko, M. Ya. Marov, “Role of hydrodynamic helicity in evolution of the protoplanetary turbulent disc”, Matem. Mod., 20:10 (2008), 99–125

Citation in format AMSBIB
\Bibitem{KolMar08} \by A.~V.~Kolesnichenko, M.~Ya.~Marov \paper Role of hydrodynamic helicity in evolution of the protoplanetary turbulent disc \jour Matem. Mod. \yr 2008 \vol 20 \issue 10 \pages 99--125 \mathnet{http://mi.mathnet.ru/mm2581} \mathscinet{http://www.ams.org/mathscinet-getitem?mr=2489471} \zmath{https://zbmath.org/?q=an:1164.85002} 

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• http://mi.mathnet.ru/eng/mm/v20/i10/p99

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Citing articles on Google Scholar: Russian citations, English citations
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This publication is cited in the following articles:
1. Kolesnichenko A.V., “On the simulation of helical turbulence in an astrophysical nonmagnetic disk”, Solar System Research, 45:3 (2011), 246–263
2. A. V. Kolesnichenko, “K teorii vikhrevogo dinamo v astrofizicheskom diske s girotropnoi turbulentnostyu”, Matem. modelirovanie, 24:4 (2012), 31–56
3. A. V. Kolesnichenko, “K teorii inversnogo kaskada energii v spiralnoi turbulentnosti astrofizicheskogo nemagnitnogo diska”, Preprinty IPM im. M. V. Keldysha, 2014, 070, 36 pp.
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