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Title: Effects of additive noise at the onset of Rayleigh-Benard convection

Journal Article · · Physical Review A. General Physics; (United States)
 [1];  [2]
  1. AT T Bell Laboratories, Murray Hill, New Jersey 07974 (United States)
  2. Department of Physics, University of Texas, Austin, Texas 78712 (United States) Center for Nonlinear Dynamics, University of Texas, Austin, Texas 78712 (United States)

The effects of additive Gaussian white noise on the onset of Rayleigh-Benard convection are studied by means of a phenomenological model, the stochastic Swift-Hohenberg equation. The strength of the noise term arising from thermal fluctuations is given for both free-slip and rigid horizontal boundaries. As was already pointed out by previous authors this term contains the small parameter [ital k][sub [ital B]T]/[rho][ital d][nu][sup 2], where [rho] is the mass density, [ital d] the plate separation, and [nu] the kinematic viscosity. For typical liquids this parameter is of order 10[sup [minus]9]. Experiments involving fluctuation effects may be interpreted in terms of this model if the noise strength is treated as an adjustable parameter, which turns out to be larger than the typical thermal value by four orders of magnitude. The effects of fluctuations on the bifurcation of an infinite system are studied, and the earlier arguments of the present authors leading to a first-order transition are reviewed [Swift and Hohenberg, Phys. Rev. A 15, 319 (1977)]. The conditions under which the multimode model can be approximated by a single-mode stochastic amplitude equation are investigated, and an earlier analytic approximation scheme for calculating the response to a time-dependent Rayleigh number is applied to the multimode model. A comparison with available experimental and numerical simulation data is presented.

DOE Contract Number:
FG05-88ER13821
OSTI ID:
7012798
Journal Information:
Physical Review A. General Physics; (United States), Vol. 46:8; ISSN 1050-2947
Country of Publication:
United States
Language:
English

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