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Mars: Occurrence of liquid water
Published online by Cambridge University Press: 14 August 2015
Abstract
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In the absence of juvenile liquid water, condensation and subsequent melting of ice are the only means of producing liquid water on the Martian surface. However, the evaporation rate is so high that the available heat sources cannot melt ice on Mars. Melting might occur only in concentrated solutions of strongly deliquescent salts.
- Type
- Part II: Mars
- Information
- Symposium - International Astronomical Union , Volume 40: Planetary Atmospheres , 1971 , pp. 247 - 250
- Copyright
- Copyright © Reidel 1971
References
Bircumshaw, L. L. and Stott, V. H.: 1929, in International Critical Tables (ed. by Washburn, E. W.), McGraw-Hill, New York.Google Scholar
Boynton, W. P. and Brattain, W. H.: 1929, in International Critical Tables (ed. by Washburn, E. W.), McGraw-Hill, New York.Google Scholar
Chapman, S. and Cowling, T. G.: 1939, The Mathematical Theory of Non-Uniform Gases, Cambridge University Press, p. 19.Google Scholar
Eckert, E. R. G. and Drake, R. M. Jr.: 1959, Heat and Mass Transfer, McGraw-Hill, New York.Google Scholar
Hall, R. E. and Sherrill, M. S.: 1929, in International Critical Tables, McGraw-Hill, New York.Google Scholar
Kliore, A., Cain, D. L., Levy, G. S., Eshelman, V. R., and Fjeldbo, C.: 1965, Science
149, 1243.CrossRefGoogle Scholar
Priestley, C. H. B.: 1959, Turbulent Transfer in the Lower Atmosphere, University of Chicago Press.Google Scholar
Spencer, H. M.: 1929, in International Critical Tables (ed. by Washburn, W. E.), McGraw-Hill, New York.Google Scholar