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Title:
Water ice cloud formation on Mars is more difficult than presumed: Laboratory studies of ice nucleation on surrogate materials
Authors:
Iraci, Laura T.; Phebus, Bruce D.; Stone, Bradley M.; Colaprete, Anthony
Affiliation:
AA(NASA Ames Research Center, Moffett Field, CA 94035, USA), AB(NASA Ames Research Center, Moffett Field, CA 94035, USA; San Jose State University, Department of Chemistry, 1 Washington Square, San Jose, CA 95192, USA), AC(San Jose State University, Department of Chemistry, 1 Washington Square, San Jose, CA 95192, USA), AD(NASA Ames Research Center, Moffett Field, CA 94035, USA)
Publication:
Icarus, Volume 210, Issue 2, p. 985-991. (Icarus Homepage)
Publication Date:
12/2010
Origin:
ELSEVIER
Abstract Copyright:
(c) 2010 Elsevier Science B.V. All rights reserved.
DOI:
10.1016/j.icarus.2010.07.020
Bibliographic Code:
2010Icar..210..985I

Abstract

The role of water ice clouds in the martian water cycle and climate depends on cloud properties such as particle size and number distribution. These properties, in turn, depend on heterogeneous nucleation parameters which are poorly understood. Here we report laboratory experiments performed under martian temperature and water partial pressure conditions (158-185 K, 9 × 10-7-1 × 10-4 Torr H2O) to determine the critical saturation ratio for ice onset, Scrit, as a function of temperature and dust composition. Using infrared spectroscopy to monitor ice nucleation and growth, we find a significant barrier to ice formation, with a pronounced temperature dependence. Even on clay minerals which show uptake of non-crystalline water before ice nucleation, we find a saturation ratio of 2.5 or more (RHice > 250%) is needed to begin ice growth at temperatures near 160 K. These results could lead to changes of four orders of magnitude in the nucleation rate relative to the presumptions used currently in Mars microphysical models, which commonly set the contact parameter, m, to a single value of 0.95. Our results range from m = 0.84 to m = 0.98. For ice nucleation on Arizona Test Dust, the temperature dependence is described by m = 0.0046 * Tnucl + 0.1085, while m = 0.0055 * Tnucl + 0.0003 on a smectite-rich clay sample. Our findings suggest that cloud formation will be more difficult than previously thought, potentially leading to areas of increased near-surface humidity but generally drier conditions in the atmosphere of Mars, overall.
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