Computer Science – Numerical Analysis
Scientific paper
Dec 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001stin...0239526p&link_type=abstract
Technical Report, JPL-Publ-01-016
Computer Science
Numerical Analysis
Solar System, Supersonics, Convection, Numerical Analysis, Computerized Simulation, Turbulence, Reynolds Number, Mach Number, Laplace Transformation, Scale Height, Kinetic Energy, Temperature Gradients
Scientific paper
A flux-corrected transport scheme is used to numerically simulate thermal convection in a two-dimensional layer of ideal, diatomic gas heated from below & stratified gravitationally across many pressure scale heights. This calculation mimics the conditions in the outer layers of the protosolar cloud [PSC] from which the Solar System formed. The temperature at the top boundary (z = 0) & a dimensionless temperature gradient of 10 at the base of the layer of thickness it are kept fixed with time. The initial atmosphere is uniformly superadiabatic, having polytropic index m = 1. Because the Reynolds number of the real atmosphere is so large, a subgrid-scale [SGS] turbulence approximation is used to model of motions whose scale is less than the computational grid size. The flow soon evolves to a network of giant convective cells spanning the whole layer. At cell boundaries the downflows are narrow & rapid while the upflows are broad & sluggish. The peak downflow Mach number is M = 1.1. The descent of the cold gas eliminates much of the initial superadiabatic structure of the lower atmosphere, so reducing the mean temperature gradient DT & causing a rise in mean density RHO towards the base. In the top 10% of depth, SGS modelling causes DART to increase sharply. A steep density inversion occurs with RHO rising to 3.5 times the initial value at the top boundary. This result gives credibility to the Modern Laplacian Theory [MLT] of Solar System origin. Here a postulated Billfold density increase at the surface of the PSC causes the shedding of discrete gas rings at the observed mean orbital spacings of the planets. Even so, further simulations that may yield M approximately 3 & a top density upturn factor of 35 are needed for the MLT to be considered valid.
Dyt C. P.
Prentice Andrew J. R.
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