Near-Surface Temperatures on Mercury and the Moon and the Stability of Polar Ice Deposits☆

@article{Vasavada1999NearSurfaceTO,
  title={Near-Surface Temperatures on Mercury and the Moon and the Stability of Polar Ice Deposits☆},
  author={Ashwin R. Vasavada and David A. Paige and Stephen E. Wood},
  journal={Icarus},
  year={1999},
  volume={141},
  pages={179-193}
}
Abstract In order to assess the thermal stability of polar ice deposits, we present model calculated temperatures of flat surfaces and surfaces within bowl-shaped and flat-floored polar impact craters on Mercury and the Moon. Our model includes appropriate insolation cycles, realistic crater shapes, multiple scattering of sunlight and infrared radiation, and depth- and temperature-dependent regolith thermophysical properties. Unshaded water ice deposits on the surface of either body are rapidly… Expand
Thermal stability of ice on Ceres with rough topography
The dwarf planet Ceres may have an ice-rich crust, and subsurface ice exposed by impacts or endogenic activity would be subject to sublimation. We model surface and subsurface temperatures on CeresExpand
Constraining the thickness of polar ice deposits on Mercury using the Mercury Laser Altimeter and small craters in permanently shadowed regions
Abstract Radar-bright deposits at the poles of Mercury are located in permanently shadowed regions, which provide thermally stable environments for hosting and retaining water ice on the surface orExpand
Age constraints of Mercury's polar deposits suggest recent delivery of ice.
TLDR
New age estimates of Mercury's polar deposits from combined analyses of Poisson statistics and direct observations of crater densities within permanently shadowed, radar-bright regions imaged by the MESSENGER spacecraft suggest that ice was delivered to Mercury within the last ~150 Myr. Expand
Stability of ice on the Moon with rough topography
Abstract The heat flux incident upon the surface of an airless planetary body is dominated by solar radiation during the day, and by thermal emission from topography at night. Motivated by the closeExpand
Thermal behavior of regolith at cold traps on the moon׳s south pole: Revealed by Chang׳E-2 microwave radiometer data
Abstract The long-term stability of water ice at cold traps depends on subsurface temperature and regolith thermophysical properties. Based on Chang׳E-2 microwave radiometer data, we have invertedExpand
New estimates for the sublimation rate for ice on the Moon
The strong hydrogen signal that the Lunar Prospector saw at the Moon's poles suggests that water ice may be present near the surface of the lunar regolith. A robotic mission to obtain in situ samplesExpand
Burial rate of Mercury's polar volatile deposits
[1] Delay Doppler images of Mercury's polar regions showing enhanced radar backscatter have been interpreted as evidence for water ice in the polar craters and are consistent with pure water iceExpand
The Lifetime of Ice on Main Belt Asteroids
We theoretically estimate the loss rate of buried ice from spherical bodies 2-3.3 AU from the Sun. The loss rate is explored as a function of about a dozen parameters. We introduce the concept of aExpand
Direct evidence of surface exposed water ice in the lunar polar regions
TLDR
Direct and definitive evidence for surface-exposed water ice in the lunar polar regions is found and the observation of spectral features of H2O confirms that water ice is trapped and accumulates in permanently shadowed regions of the Moon and in some locations, it is exposed at the modern optical surface. Expand
The role of atmospheric pressure on Mars surface properties and early Mars climate modeling
Abstract The thermal inertia of a planetary surface is a compound function of the regolith thermal conductivity, density and specific heat. On planetary bodies with atmospheres, the conductivity ofExpand
...
1
2
3
4
5
...

References

SHOWING 1-10 OF 57 REFERENCES
The Thermal Stability of Water Ice at the Poles of Mercury
TLDR
Thermal model calculations show that, despite Mercury's proximity to the sun, the temperatures of flat, low-reflectivity surfaces at Mercury's poles are not expected to exceed 167 kelvin, which is consistent with the presence of water ice. Expand
Near-Surface Ice on Mercury and the Moon: A Topographic Thermal Model
Abstract A thermal model that can be easily adapted to craters of arbitrary shape is developed and applied to high-latitude impact craters on Mercury and the Moon, Chao Meng Fu crater at -87.5°L onExpand
Temperature variations across craters in the polar regions of the Moon and Mercury
Abstract Temperatures in the permanently shadowed regions inside the craters on the Moon and Mercury are re-examined by taking into account the wavelength and directional dependences of albedo andExpand
Lunar cold traps and their influence on argon-40
In polar areas of the moon the maximum temperatures reached in some permanently shaded areas are well below the temperature required to retain water ice for billions of years, and cold enough to holdExpand
Surface brightness temperatures at the Apollo 17 heat flow site - Thermal conductivity of the upper 15 cm of regolith
Lunar surface brightness temperatures derived as part of the Apollo 17 heat flow experiment are reported. Nighttime surface temperatures, calculated from the data provided by two thermocouplesExpand
Mercury's polar caps and the generation of an OH exosphere
Abstract We predict the OH column that will be present in the polar regions of the mercurian exosphere for physically realistic ice deposits at the poles, including both surface and buried ice. TheExpand
Stability of polar frosts in spherical bowl-shaped craters on the Moon, Mercury, and Mars
Following Svitek (Martian Water Frost: Control of Global Distribution by Small-Scale Processes, Ph.D Thesis, California Institute of Technology, 1992), analytic solutions are presented for theExpand
The migration of volatiles on the surfaces of Mercury and the Moon
Radar observations of Mercury have provided the startling discovery of the probable existence of substantial deposits of ices in permanently shaded polar regions [Butler et al., 1993; Harmon et al.,Expand
Thermophysics of the planet Mercury
Recent observations of the thermal emission of Mercury at microwave and infrared frequencies now permit a determination of the thermal and electrical properties of the subsurface of the planet. RadarExpand
Sulfur at Mercury, Elemental at the Poles and Sulfides in the Regolith
We propose that the bright radar spots seen at Mercury's north and south poles are a result of volume scattering from elemental sulfur. Further we suggest that the high average index of refractionExpand
...
1
2
3
4
5
...