Convective stability of a layer of magnetizable liquid with solid boundaries

1978 ◽  
Vol 35 (2) ◽  
pp. 973-978 ◽  
Author(s):  
E. G. Bashtovoi ◽  
M. I. Pavlinov
Keyword(s):  
Convective Stability ◽  
Magnetizable Liquid

Energy method in the theory of convective stability of a non-Newtonian liquid

1979 ◽  
Vol 15 (3) ◽  
pp. 179-185
Author(s):  
F. A. Garifullin ◽  
K. Z. Galimov
Keyword(s):  
Energy Method ◽  
Newtonian Liquid ◽  
Convective Stability

Convective Stability of Galaxy‐Cluster Plasmas

2006 ◽  
Vol 642 (1) ◽  
pp. 140-151 ◽  
Author(s):  
Benjamin D. Chandran ◽  
Timothy J. Dennis
Keyword(s):  
Galaxy Cluster ◽  
Convective Stability

Shrinkage flow effects on the convective stability of NH4Cl-H2O directional solidification

AIAA Journal ◽  
1995 ◽  
Vol 33 (8) ◽  
pp. 1531-1534 ◽  
Author(s):  
J. A. Hopkins ◽  
T. D. McCay ◽  
M. H. McCay
Keyword(s):  
Directional Solidification ◽  
Convective Stability ◽  
Flow Effects

Experimental investigation of convective stability in a superposed fluid and porous layer when heated from below

1989 ◽  
Vol 207 ◽  
pp. 311-321 ◽  
Author(s):  
Falin Chen ◽  
C. F. Chen
Keyword(s):  
Porous Layer ◽  
Fluid Layer ◽  
Critical Rayleigh Number ◽  
Linear Stability Theory ◽  
Convective Stability ◽  
Onset Of Convection ◽  
Temperature Distributions ◽  
Critical Wavelength ◽  
Crystal Film ◽  
Flux Curve

Experiments have been carried out in a horizontal superposed fluid and porous layer contained in a test box 24 cm × 12 cm × 4 cm high. The porous layer consisted of 3 mm diameter glass beads, and the fluids used were water, 60% and 90% glycerin-water solutions, and 100% glycerin. The depth ratio ď, which is the ratio of the thickness of the fluid layer to that of the porous layer, varied from 0 to 1.0. Fluids of increasingly higher viscosity were used for cases with larger ď in order to keep the temperature difference across the tank within reasonable limits. The top and bottom walls were kept at different constant temperatures. Onset of convection was detected by a change of slope in the heat flux curve. The size of the convection cells was inferred from temperature measurements made with embedded thermocouples and from temperature distributions at the top of the layer by use of liquid crystal film. The experimental results showed (i) a precipitous decrease in the critical Rayleigh number as the depth of the fluid layer was increased from zero, and (ii) an eightfold decrease in the critical wavelength between ď = 0.1 and 0.2. Both of these results were predicted by the linear stability theory reported earlier (Chen & Chen 1988).

Origin and Evolution of Wolf-Rayet Stars

1982 ◽  
Vol 99 ◽  
pp. 377-381
Author(s):  
A. Tutukov ◽  
L. Yungelson
Keyword(s):  
Mass Loss ◽  
Massive Stars ◽  
Close Binary ◽  
Initial Mass ◽  
Convective Stability ◽  
Helium Burning ◽  
Origin And Evolution ◽  
The Core

The larger part of close binary components with initial mass exceeding ∼20 Mo becomes WR stars in the core helium burning stage. Some of the most massive WR stars may be products of evolution of single massive stars with initial masses exceeding ∼50 M0 if the mass loss in the infrared supergiant stage is effective enough. The Ledoux criterion of convective stability seems more promising to explain the observed properties of WR stars.

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