Download Convection in Rotating Fluids by B. M. Boubnov, G. S. Golitsyn (auth.) PDF
By B. M. Boubnov, G. S. Golitsyn (auth.)
Spatial inhomogeneity of heating of fluids within the gravity box is the reason for all motions in nature: within the surroundings and the oceans in the world, in astrophysical and planetary items. All average gadgets rotate and convective motions in rotating fluids are of curiosity in lots of geophysical and astrophysical phenomena. in lots of business functions, too (crystal development, semiconductor manufacturing), heating and rotation are the most mechanisms defining the constitution and caliber of the fabric.
looking on the geometry of the structures and the mutual orientation of temperature and gravity box, various phenomena will come up in rotating fluids, equivalent to typical and oscillating waves, extensive solitary vortices and general vortex grids, interacting vortices and turbulent blending. during this booklet the authors elucidate the actual essence of those phenomena, identifying and classifying stream regimes within the house of similarity numbers. The theoretical and computational effects are provided merely while the implications support to give an explanation for uncomplicated qualitative movement features.
The booklet could be of curiosity to researchers and graduate scholars in fluid mechanics, meteorology, oceanography and astrophysics, crystallography, warmth and mass move.
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Extra resources for Convection in Rotating Fluids
Sample text
Rolls, Benard cells, etc. In rotating fluids, besides the monotonic mode there is also an oscillatory mode. It formally exists in the case n = 0, but the critical Rayleigh number for it is higher than for the monotonic one, so it never develops in reality. 12) this mode requires (j =f O. 21 ) = (;;-) 2 = (¥)\s determined by a solution of the following equation 2x 3 + 3x 2 = 1+ Pr 2 (1 + Pr 2) -1 7r- 4 Ta. 22) It is immediately clear that for Pr'2 1 the oscillatory mode does not exist. 677. At Pr E. the difference between the critical values of the Rayleigh numbers is decreasing with the increase of the Taylor number, but no intersection of the curves occurs. fO 6 To.. --J o 10 4 fOB (0 '2 10 (6 fO'lO Figure 3: Dependence of critical Rayleigh number Ra CT on Taylor number Ta for different boundary conditions (see text). Arrows indicate the different axis for the Rayleigh number. (After Boubnov & Senatorsky, 1989a). At large Taylor numbers (practically at Ta > 106 ), all critical curves have the same asymptotes: 2 Ra CT = k R . The case of stationary convection in a rotating fluid, were carried The structure of the convective motions and at small supercriti'cal Rayleigh numbers 39 out by Fultz et al (1954,1955). A special attention was paid to the mercury free upper surface. Because it is oxidized rather quickly, it behaves largely as a rigid upper surface with constant temperature. For determining the critical Rayleigh number, the gradient method was used. Further results were obtained by T. Rossby (1969) which are represented in Fig.