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Through this link, a more fundamental understanding of the geology, stratigraphy, and internal structure of Vesta’s preserved ancient planetary surface will be achieved. The observations identified above require mobility, either for sampling of multiple surface and subsurface units on a heterogeneous asteroid such as Vesta, or for positioning geophysical instruments that must work in tandem. Horizontal mobility also could provide vertical mobility by sampling blocks excavated by impact craters.

Schubert, “Penetrative Convection and Zonal Flow on Jupiter,” Science 273: 941, 1996. 54. , 1994, pp. 61, 80, 93. 55. B. T. B. McCord, “Galilean Satellites: Identification of Water Frost,” Science 178: 1087, 1972. 56. U. H. P. Larson, “Infrared Spectra of the Galilean Satellites of Jupiter,” Astrophysical Journal 179: L154, 1973. 57. G. , 1998 (CD-ROM). 58. R. , 1998 (CD-ROM). 59. K. Zahnle, H. Levison, and L. , 1998 (CD-ROM). 60. D. , “Europa’s Differentiated Internal Structure: Inferences from Two Galileo Encounters,” Science 276: 1236, 1996.

Subsequent missions would emplace more sophisticated balloons capable of descending deep into Jupiter’s atmosphere and/or balloons with the ability to release dropsondes. In either case, it is likely that the latter balloons or dropsondes would need to survive to pressure depths of some 100 bars, that is, four to five times that experienced by Galileo’s probe. The primary factors determining the required lifetimes of the balloons are the wind speeds. These vary greatly Copyright © National Academy of Sciences.

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