Behavior of Carbon Dioxide and Other Volatiles on Mars

  title={Behavior of Carbon Dioxide and Other Volatiles on Mars},
  author={Robert B. Leighton and Bruce C. Murray},
  pages={136 - 144}
We have found that a rather simple thermal model of the Martian surface, in combination with current observations of the atmospheric composition, points strongly toward the conclusion that the polar caps of Mars consist almost entirely of frozen CO2. This study was based upon the following principal assumptions. 1) Carbon dioxide is a major constituent of the Martian atmosphere. 2) The blanketing effect of the atmosphere is small, and due principally to the absorption band of CO2 near 15… 
Mineral stability at the Martian surface
Thermodynamic calculations of mineral stability fields under a range of predicted surface conditions for Mars indicate that goethite will be unstable except under the wettest and coldest parts (pH2O
Polar Volatiles on Mars—Theory versus Observation
The residual frost caps of Mars are probably water-ice and a permanent reservoir of solid CO2 is also probably present within the north residual cap, which may comprise a mass of CO2 some two to five times that of the present atmosphere of Mars.
Seasonal carbon dioxide exchange between the regolith and atmosphere of Mars: Experimental and theoretical studies
Measurements of the rate of penetration of a CO2 ‘pressure wave’ through basalt-clay soils have been conducted under conditions of PCO2 (∼6 mbar), ΔPCO2 (∼2 mbar), soil density (ρ ∼ 1.3), and T (−40°
Numerical Experiment of Radiative-Convective Equilibrium of the Martian Atmosphere
Temperature distributions and its diurnal changes in the Martian atmosphere are computed numerically under a radiative-convective equilibrium. Especially, the green house effect of H2O having the
Modeling studies related to carbon dioxide phase change on Mars
  • Xin Guo
  • Environmental Science, Physics
  • 2009
Carbon dioxide (CO₂) is the most abundant gaseous species in the atmosphere of Mars. Phase change of CO₂, predominantly between gas and solid, is the most eminent feature in the current Martian
Origin of planetary atmospheres
The near absence of noble gases on earth, other than those of radioactive origin, indicates that the earth was formed by the accumulation of planetesimals; this process systematically excluded all
Carbon 14 measurements of the Martian atmosphere as an indicator of atmosphere‐regolith exchange of CO2
A determination of the mixing ratio of 14CO2 in the Martian atmosphere would provide a direct measurement of the degree of exchange of CO2 in the Martian atmosphere with CO2 in the regolith and polar
A model for the hydrologic and climatic behavior of water on Mars
Past studies of the climatic behavior of water on Mars have universally assumed that the atmosphere is the sole pathway available for volatile exchange between the planet's crustal and polar


The behavior of volatiles on the lunar surface
Volatiles, and water in particular, have been thought to be unstable on the lunar surface because of the rapid removal of constituents of the lunar atmosphere by solar radiation, solar wind, and
Atmosphere of Mars
The Martian ionospheric observations made by Mariner IV are interpreted in terms of an atmospheric model. The ion peak is identified as an F2 peak, that is, as a maximum whose profile is controlled
Mars is the only planet whose surface features can be observed in detail. Because its diurnal and seasonal changes are similar to those of the earth, it has been reasonable to attempt an explanation
Origin and evolution of atmospheres and oceans
In recent years it has become evident that the atmosphere and oceans have been produced by the outgassing of volatile materials from the earth's interior, principally from volcanoes. In 1950 W. W.
An analysis of the spectrum of mars
On a high-dispersion spectrogram of Mars taken at Mount Wilson rotational lines of H_2O near λ 8300 and CO_2 near λ 8700 have been detected. Recent laboratory measurements of line strengths by D.
Occultation Experiment: Results of the First Direct Measurement of Mars's Atmosphere and Ionosphere
Preliminary analysis of changes in the frequency, phase, and amplitude of the Mariner IV radio signal, caused by passage through the atmosphere and ionosphere of Mars, have yielded estimates of the refractivity and density of the atmosphere near the surface, the scale height in the atmosphere, and the electron density profile of the Martian ionosphere.
Radio Observations of Mars
THERMAL radio emission from Mars was first detected by Mayer, McCullough and Sloanaker during the favourable opposition of 1956 at 3.15 cm (ref. 1). Further observations at this wave-length made near
Mars: Upper Atmosphere
The thermal structure of the upper atmosphere of Mars has been theoretically investigated and the exospheric temperature lies between 400� and 700�K, for a pure CO2 model atmosphere.