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Polar Volatiles on Mars—Theory versus Observation - Excess solid carbon dioxide is probably present in the north residual cap

Murray, Bruce C. and Malin, Michael C. (1973) Polar Volatiles on Mars—Theory versus Observation - Excess solid carbon dioxide is probably present in the north residual cap. Science, 182 (4111). pp. 437-443. ISSN 0036-8075. doi:10.1126/science.182.4111.437.

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The residual frost caps of Mars are probably water-ice. They may be the source of the water vapor associated with seasonal polar hoods. A permanent reservoir of solid CO_2 is also probably present within the north residual cap and may comprise a mass of CO_2 some two to five times that of the present atmosphere of Mars. The martian atmospheric pressure is probably regulated by the temperature of the reservoir and not by the annual heat balance of exposed solid CO_2 (37). The present reservoir temperature presumably reflects a long-term average of the polar heat balance. The question of a large permanent north polar cap is reexamined in light of the Mariner 9 data. The lower general elevation of the north polar region compared to the south and the resulting occurrence in the north of a permanent CO_2 deposit are probably responsible for the differences in size and shape of the two residual caps. The details of the processes involved are less apparent, however. It might be argued that the stability of water-ice deposits depends on both insolation and altitude. The present north and south residual caps should be symmetrically located with respect to such a hypothetical stability field. However, the offset of the south cap from the geometrical pole, the non-symmetrical outline of the north cap, and the apparently uniform thickness of the thin, widespread water-ice all argue against control by simple solid-vapor equilibrium of water under present environmental conditions. We think that the present location of the water-ice may reflect, in part, the past location of the permanent CO_2 reservoir. The extreme stability of polar water-ice deposits increases the likelihood that past environmental conditions may be recorded there. Detailed information on elevations in the vicinity of the residual caps is needed before we can further elucidate the nature and history of the residual caps. This, along with measurements of polar infrared emission, should be given high priority in future missions to Mars. Two conclusions follow from the limitation of the mass of solid CO_2 on Mars at present to two to five times the mass of CO_2 in the atmosphere. If all of this CO_2 was entirely sublimated into the atmosphere as a result of hypothetical astronomical or geophysical effects, the average surface pressure would increase to 15 to 30 mbar. Although such a change would have considerable significance for eolian erosion and transportation, there seems to be little possibility that a sufficiently earthlike atmosphere could result for liquid water to become an active erosional agent, as postulated by Milton (38). The pressure broadening required for a green-house effect requires at least 10 to 20 times more pressure (39). If liquid water was ever active in modifying the martian surface, it must have been at an earlier epoch, before the present, very stable CO_2/H_2O system developed. There can be no intermittent earthlike episodes now. Furthermore, the present abundance of CO_2 on Mars may be an indicator of the cumulative evolution of volatiles to the surface of the planet (40). Thus, even the possibility of an earlier earth-like episode is dimmed. On Mars, the total CO_2 definitely outgassed has evidently been about 60 ± 20 g/cm^2. On the earth, about 70 ± 30 kg/cm^2 of CO_2 have been released to the surface (41). Hence, the total CO_2 devolved by Mars per unit area is about 0.1 percent of that evolved by the earth. Thus, the observational limits we place on solid CO_2 presently located under the north residual cap also may constitute considerable constraints on the total differentiation and devolatilization of the planet. If they are valid, it would seem unlikely that Mars has devolatilized at all like the earth, or ever experienced an earthlike environment on its surface.

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Additional Information:© 1973 American Association for the Advancement of Science. We wish to acknowledge G. Biggs and J, Cutts of Jet Propulsion Laboratory, Pasadena; A. P. Ingersoll, R. B. Leighton, and R. P. Sharp of California Institute of Technology, Pasadena; and H. Kieffer of the University of California at Los Angeles for discussions, criticisms, and helpful debates concerning early drafts of this paper. S. C. Yeung, Princeton University, contributed to the early development of some of the ideas presented here. Supported in part by the National Aeronautics and Space Administration. Contribution No. 2248 of the Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena 91109.
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Caltech Division of Geological and Planetary Sciences2248
Issue or Number:4111
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Official Citation:Polar Volatiles on Mars—Theory versus Observation Bruce C. Murray and Michael C. Malin Science 2 November 1973: 182 (4111), 437-443. [DOI:10.1126/science.182.4111.437]
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:55185
Deposited By: Tony Diaz
Deposited On:25 Feb 2015 20:16
Last Modified:10 Nov 2021 20:42

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