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By W. B. Olstad

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The present code, without density in the expression for the mixing length, is in very good agreement with the data, closer than any of the others. The predictions obtained with density in the mixing length equation significantly exceed the data. The other predictions shown in Fig. 23 BLIMP is a well-developed and widely used nonradiating boundary layer prediction technique which has, as alternative options, the mixing length models of Ken da 11. et a l . 24 it is immediately evident that the turbulent models with density, both the Kendall and the present model, significantly overpredict highly cooled wall boundary-layer heat transfer.

Purchased from American Institute of Aeronautics and Astronautics 32 W. E. NICOLETAND A. BALAKRISHNAN log y Fig. 2 Schematic of velocity profile in turbulent flow illustrating w a l l - l a w and wake-law regions. This latter assumption is disputed by limited experimental evidence? suggesting that the entire shock layer becomes turbulent if the blowing is hard enough. Once transition occurs, the growth of the mixing layer should be qualitatively similar to that of a turbulent shear layer flowing between two parallel inviscid shear flows.

5b), the heating rate is negligible for coupled laminar flow and never exceeds 14% of the no-injection, turbulent value for coupled turbulent flow. Figures 6 through 11 present results for several flow parameters that help to explain why turbulence produces increased surface radiative heating. Figures 6 through 9 also contrast the differences between the sphere cone and hyperboloid results. Because of the large surface-heating rates for Jupiter entry, the coupled carbon-phenolic injection rate is large, as evidenced by the mass injection distribution rates shown in Fig.

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