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  • 1
    Electronic Resource
    Electronic Resource
    Springer
    The European physical journal 15 (1990), S. 71-78 
    ISSN: 1434-6079
    Keywords: 31.20
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Variational (≃30 000 determinants) and perturbational (≃3.5 million determinants) Localized Multireference Configuration Interaction (LMRCI) calculations includingf polarization functions are made to study the role played by the three-body terms in the stabilization energy of three selected geometries of the silver trimer: linear, equilateral and a Jahn-Teller obtuse triangle conformation. A comparative analysis of the relative stability of these geometries is done through a many-body decomposition of the interaction energy. Like in Cu3, the most symmetrical arrangement (i.e. an equilateral triangle) is found to be less stable than the obtuse triangle because it has the highest three-body repulsion energy. The absolute minimum is the obtuse triangle having a Jahn-Teller stabilization energy of 328 cm−1. Unlike Cu3, the linear geometry is found to be less stable than the equilateral by 1282cm−1. Results show again the importance of three-body terms in the total interaction energy of these trimers.
    Type of Medium: Electronic Resource
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  • 2
    facet.materialart.
    Unknown
    In:  CASI
    Publication Date: 2013-08-31
    Description: Analyzing turbulent flows with rotation, Dubrulle and Valdettaro have concluded that some new effects come into play and may modify the standard picture we have concerning turbulence. In that respect the value of the Rossby number is of crucial importance since it will determine the transition between regimes where rotation is or is not important. With rotation there will be a tendency to constrain the motion to the plane perpendicular to the rotation axis and as a consequence the horizontal scale will increase as compared to the longitudinal one, which means that the turnover time in this direction will increase. The net effect is that the energy cascade down process is hindered by rotation. As a matter of fact, when rotation is present one observes two cascades: an enstrophy (vorticity) cascade from large scales to small scales; and an inverse energy cascade from small scales to large scales. Since the first process is not efficient on transporting energy to the dissipation range, what we see is energy storage in the large structures at the expense of the small structures. This kind of behavior has been confirmed experimentally. For a very large gamma we obtain, in the inertial range, a spectrum of k(exp -3) instead of the usual Kilmogorov's k(exp -5/3) spectrum. In reality, when rotation is dominant, energy gets stored in inertial waves that propagate it essentially in the longitudinal direction. In that case, we can no longer assign just one viscosity to the fluid and, what is most important, the concept of viscosity loses its meaning since we no longer have local transport of energy. Such results, however, were derived considering a hot disk, in which opacity is mainly given by electron scattering. In the present work we have applied the formulation developed in the previous work for the description of the viscous-stage solar nebula.
    Keywords: SOLAR PHYSICS
    Type: Lunar and Planetary Inst., Workshop on Physics of Accretion Disks Around Compact and Young Stars; p 4
    Format: application/pdf
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  • 3
    facet.materialart.
    Unknown
    In:  Other Sources
    Publication Date: 2019-01-25
    Description: It is widely believed that a primordial solar nebula, the precursor of the Sun and its planetary system, could be best described in terms of an accretion disk. Such an accretion disk is though to be turbulent, and it is usually imagined that turbulent viscosity alone provides the torque responsible for the structure and the evolution of the nebula. However, it was found that an MHD dynamo operating in a turbulent nebula can contemporaneously produce magnetic fields capable of significantly altering or even dominating the total torque. Thus, it seems that no model of a viscous solar nebula is complete without taking magnetic fields into consideration. It was demonstrated that there are usually two distinct regions of nebular disk where a dynamo can operate: the inner region, where the magnetic field coupled to gas due to relatively high thermal ionization; and the outer region, where this coupling is achieved due to nonthermal ionization. Most models also show the existence of an intermediate region, 'the magnetic gap,' where neither thermal nor nonthermal sources can produce enough ionization to provide the necessary coupling between the magnetic field and the gas. The location and width of the gap change substantially from one model to another. At present, we can only estimate the strength of a generated magnetic field. It seems that a large-scale magnetic field is likely to be in the equipartition with the turbulent kinetic energy; however, the intense magnetic fluctuations may greatly exceed this equipartition strength on short time and length scales. To show how a dynamo-generated magnetic field changes the structure of a viscous nebula, we consider four nebula models extensively.
    Keywords: SOLAR PHYSICS
    Type: Twenty-Fourth Lunar and Planetary Science Conference. Part 3: N-Z; p 1351-1352
    Format: text
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