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By G. A. Soffen (auth.), George Marx (eds.)

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Additional resources for Bioastronomy — The Next Steps: Proceedings of the 99th Colloquium of the International Astronomical Union held in Balaton, Hungary, June 22-27, 1987

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For further details see the papers referred above. There were also particles out of these classes. Their spectra need further investigations. In three cases the analyses can not exclude the presence of pure ice particles. 11. , Astron. , to be publ ished 1987). 11. 99,1982. , Icarus 64, 51, 1986. , The Astrophys. J. 278, 449, 1984. , 5, 233, 1985. 11. 269, 1986. II. 255, 1986. 1. 397, 1986. , Nature 321, 320, 1986. , Catalog. of comet. orbits, Cambridge, 1982. , 10, 1, 1985. , Icarus 54, 388, 1983.

What prevents an excessive progression of oxidation is the vapourization of water. erials. osynthesis regenerates carbohydrate. For photosynthesis to proceed, several hundred moles of water, which do not appear in the chemical equation, are needed per the molar chemical equation 6C02+6H20~C6H1206+602' The glucose prooduced is a materia I with high energy and low entropy. The Sun's light fixed as chemical energy has made it high energy, while the water, vapourized and escaping through stomata, has made it low entropy.

Geothermal energy could also make a significant contribution. While an environment in which life could actually evolve is unlikely in our solar system, other solar systems could have considerably more optimum conditions. Furthermore, if a large natural satellite could form with an atmosphere and undergo sufficient tidal heating over its history that its surface would be maintained above freezing, life could conceivably evolve there. In this paper, we examine the prospects for aqueous environments on satellites in the outer solar system.

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