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Published Online: 15 October 2019
Accepted: September 2019

Computational fluid radiative dynamics of the Galileo Jupiter entry featured

Physics of Fluids 31, 106104 (2019); https://doi.org/10.1063/1.5115264
L. Santos Fernandes1,a), B. Lopez2,b), and M. Lino da Silva1,c)
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Abstract
On December 7th, 1995, the Galileo descent probe entered Jupiter’s atmosphere at a relative velocity of 47.4 km s−1. Flight data revealed an unforeseen recession profile: while the stagnation region had been significantly oversized, the shoulder almost completely ablated. In an attempt to understand why numerical predictions diverge from the flight data, several sensitivity studies were performed at the 180 km altitude point. The inaccuracy of the Wilke/Blottner/Eucken model at temperatures above 5000 K was confirmed. When applied to Galileo’s entry, it predicts a narrower shock with higher peak temperatures compared to the Gupta/Yos model. The effects of He and H2 line-by-line radiation were studied. Inclusion of these systems increased radiative heating by 9% at the stagnation point, even when precursor heating is unaccounted for. Otherwise, the internal excitation of H2 due to absorption of radiation originating from the highly emitting shock layer promotes H2 emission before dissociation occurs at the shock, yielding 196% higher radiative heat fluxes. This emphasizes the importance of H2 radiation not only on the recession experienced by Galileo but also for future entries in gas giants. Accordingly, thermal nonequilibrium resulted in 25% lower radiative heating when compared to an equilibrium solution, contrary to previous investigations that neglected H2. Ablation products absorption was shown to counteract the increased emission due to precursor heating of H2. However, the ablation layer temperature must be accurately predicted using a material-response code coupled to the flowfield since radiative heating has been shown to significantly depend on this energy-exchange interaction. Finally, the tangent-slab and ray-tracing models agreed to within 12%.

ACKNOWLEDGMENTS

M. Lino da Silva’s work has been funded by the Portuguese FCT–Fundação para a Ciência e Tecnologia through the Project No. UID/FIS/50010/2019. The authors would like to thank Markus Fertig for the thoughtful suggestions regarding the modeling of shoulder expansion and Domenico Bruno for general comments about this work, provided during the European Space Agency-sponsored 8th International Workshop on Radiation of High Temperature Gases.

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