Stellar convection as a low Prandtl number flow

Author(s):  
Josep M. Massaguer
1991 ◽  
Vol 130 ◽  
pp. 57-61
Author(s):  
Josep M. Massaguer

AbstractThermal convection in the Sun and cool stars is often modeled with the assumption of an effective Prandtl number σ ≃ 1. Such a parameterization results in masking of the presence of internal shear layers which, for small σ, might control the large scale dynamics. In this paper we discuss the relevance of such layers in turbulent convection. Implications for heat transport – i.e. for the Nusselt number power law – are also discussed.


2017 ◽  
Vol 10 (3) ◽  
pp. 778-784
Author(s):  
Sanjin Saric ◽  
Andreas Ennemoser ◽  
Branislav Basara ◽  
Heinz Petutschnig ◽  
Christoph Irrenfried ◽  
...  

2010 ◽  
Vol 1 (1-2) ◽  
pp. 15-20 ◽  
Author(s):  
B. Bolló

Abstract The two-dimensional flow around a stationary heated circular cylinder at low Reynolds numbers of 50 < Re < 210 is investigated numerically using the FLUENT commercial software package. The dimensionless vortex shedding frequency (St) reduces with increasing temperature at a given Reynolds number. The effective temperature concept was used and St-Re data were successfully transformed to the St-Reeff curve. Comparisons include root-mean-square values of the lift coefficient and Nusselt number. The results agree well with available data in the literature.


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