Dust collapse occurs in a subset of high disc mass simulations, The ability of the spiral structures to concentrate solids increases with theĬooling time, and decreases with the Stokes number, while the relativeĭynamical temperature between gas and dust of the particles decreases with theĬooling time and the disc-to-star mass ratio, and increases with the Stokes Instability of the simulated discs is sustained by local cooling. Strength of gravitational instability, and the Stokes number. How the formation of solid clumps depends on the disc-to-star mass ratio, the Three-dimensional smoothed particle hydrodynamics simulations of two-fluidĭiscs, in the regime where the Stokes number of the particles St>1, to study The Class 0/I stages of Young Stellar Object evolution. In otherwise non-fragmenting gas discs, forming Earth-mass solid cores during ThisĬombination could lead to short-wavelength fragmentation of the solid component Support grain growth to sizes where the particles decoupled from the gas. Numerical simulations, by Cristiano Longarini and 4 other authors Download PDF Abstract: Young protostellar discs are likely to be both self-gravitating, and to Download a PDF of the paper titled The role of the drag force in the gravitational stability of dusty planet-forming disc - II.
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