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We analyze Phoenix Thermal and Electric Conductivity Probe (TECP) instrument data and previous experimental data to present constraints on the parameters for regolith-driven adsorption at the Phoenix landing site. Modeling Brunauer–Emmett–Teller (BET) adsorption of the data across Mars-relevant materials yielded fairly constant surface coverage and enthalpy values, θ = 0.336, corresponding to 2.96...
We analyze the recalibrated in situ humidity measurements by the Phoenix lander, which landed at 68.2°N, 234.3°E and operated from Ls 78° through Ls 148°, ∼152 sols. Vapor pressures demonstrate significant day–night variations with values ranging from 0.005Pa to 0.37Pa, an order of magnitude lower than previously reported, and evening derived enthalpies less than that for a purely ice deposition-driven...
Saturn’s moon Iapetus has an equatorial ridge system, which may be as high as 20km, that may have formed by endogenic forces, such as tectonic and convective forces, or exogenic processes such as debris infall. We use high-resolution topographic data to conduct a topographic analysis of the ridge, which suggests a predominantly triangular morphology, with some ridge face slopes reaching 40°, allowing...
Remote sensing data suggest Mercury's surface has compositional variations spatially associated with crater and basin ejecta, the so-called “Low-Reflectance Material” (LRM), which has been suggested to be enriched in a subsurface native darkening agent that is excavated and redeposited onto the surface. This unit may record the evidence of impact-induced mixing of Mercury's outer layers during its...
CRISM indicates the presence of water ice patches in Richardson crater, located on Mars’ southern polar region at the area of the seasonal ice cap. Numerical simulations suggest that the maximum daytime temperature of the ice at these locations is between 195 and 220K during local spring. Previous studies suggest that at these temperatures liquid interfacial water could be present. Here, for the first...
It has been shown through both measurements and simulations that there exists a measurable ice-free, porous, overburden overlaying water ice on Cassini Regio. Mass transfer through this porous media in a vacuum would occur in the Knudsen regime, which provides sublimation rates orders of magnitude smaller than Hertz–Langmuir sublimation. The availability of water ice for transport from this region...
The energy balance at the surface of an airless planetary body is strongly influenced by the bolometric Bond albedo and the surface thermal inertia. Both of these values may be calculated through the application of a thermal model to measured surface temperatures. The accuracy of either, though, increases if the value of the other is better constrained. In this study, we used the improved global bolometric...
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