A Caltech Library Service

A geologic evaluation of thermal properties for the elysium and aeolis quadrangles of Mars

Zimbelman, James R. and Leshin, Laurie A. (1987) A geologic evaluation of thermal properties for the elysium and aeolis quadrangles of Mars. Journal of Geophysical Research D, 92 (B4). E588-E596. ISSN 0148-0227. doi:10.1029/jb092ib04p0e588.

[img] PDF - Published Version
See Usage Policy.


Use this Persistent URL to link to this item:


Thermal inertias with spatial resolutions as small as 2 by 5 km were combined in a regional study of the Elysium and Aeolis quadrangles of Mars (30°N to 30°S, 180°W to 225°W). The range of thermal inertias obtained was 1–14 (× 10⁻³ cal cm⁻² s^(−½) K⁻¹ = 41.84 j m⁻² s^(−½) K⁻¹), with the lowest values corresponding to the Elysium Rise and the highest values correlating with dark patches of aeolian material in the southern highlands. The thermal properties obtained from the high spatial resolution measurements are essentially identical to the results obtained from data with much poorer spatial resolution, indicating a regional homogeneity of surface properties at scales greater than 5 km. Aeolian features, both dark patches and bright materials associated with topographic obstacles such as craters, have higher thermal inertias than do their surroundings. Other surface features do not display distinctive thermal properties, even when clearly resolved from their surroundings. Comparison of the thermal inertias with global data sets shows a pronounced inverse correlation with albedo (consistent with globally observed trends) and brightnesses at red, green, and violet wavelengths but no prominent correlation with elevation. Thermal inertias for individual geologic units within the two quadrangles appear to be more strongly controlled by the location of the terrain in either the northern plains or the southern highlands than by properties intrinsic to the unit.

Item Type:Article
Related URLs:
URLURL TypeDescription
Zimbelman, James R.0000-0002-0420-8453
Additional Information:The authors wish to thank P. Christensen and H. Kieffer for careful reviews of the original version of the manuscript; their comments and suggestions were most helpful in revising the manuscript. This research was supported while J. Z. was a Visiting Post-Doctoral Fellow and L. L. was a 1985 Visiting Undergraduate Intern at the Lunar and Planetary Institute, which is operated by the Universities Space Research Association under Contract No. NASW-4066 with the National Aeronautics and Space Administration. In addition, L. L. was provided travel support by the Planetary Geology Undergraduate Research Program to present these results at the 17th Lunar and Planetary Science Conference. This paper is LPI Contribution No. 611.
Funding AgencyGrant Number
Lunar and Planetary InstituteUNSPECIFIED
Arizona State UniversityUNSPECIFIED
Issue or Number:B4
Record Number:CaltechAUTHORS:20230307-650546000.65
Persistent URL:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:119778
Deposited By: George Porter
Deposited On:08 Mar 2023 18:16
Last Modified:08 Mar 2023 18:16

Repository Staff Only: item control page