Yamamoto, Masaru Ikeda, Kohei Takahashi, Masaaki
Published in
Icarus
Thermal tides, stationary waves, and general circulation are investigated using a T63 Venus general circulation model (GCM) with solar and thermal radiative transfer in the presence of high-resolution surface topography, based on time average analysis. The simulated wind and static stability are very similar to the observed ones (e.g., Horinouchi e...
Wiens, Roger C Edgett, Kenneth S Stack, Kathryn M Dietrich, William E Bryk, Alexander B Mangold, Nicolas Bedford, Candice Gasda, Patrick Fairen, Alberto Thompson, Lucy
...
Published in
Icarus
Heterolithic, boulder-containing, pebble-strewn surfaces occur along the lower slopes of Aeolis Mons ("Mt. Sharp") in Gale crater, Mars. They were observed in HiRISE images acquired from orbit prior to the landing of the Curiosity rover. The rover was used to investigate three of these units named Blackfoot, Brandberg, and Bimbe between sols 1099 a...
Brossier, Jeremy Gilmore, Martha S.
Published in
Icarus
Numerous studies show that major Venus highlands display anomalously high radar reflectivity and low radar emissivity relative to the planetary average. This is thought to be the result of the formation of minerals having high dielectric constants via weathering reactions occurring between the surface and the deep atmosphere in these elevated terra...
Wright, Esteban Quillen, Alice South, Juiliana Nelson, Randal C. Sanchez, Paul Siu, John Askari, Hesam Nakajima, Miki Schwartz, Stephen R.
Spin off events and impacts can eject boulders from an asteroid surface and rubble pile asteroids can accumulate from debris following a collision between large asteroids. These processes produce a population of gravitational bound objects in orbit that can impact an asteroid surface at low velocity and with a distribution of impact angles. We pres...
Dundas, Colin M
Published in
Icarus
Recurring Slope Lineae (RSL) on Mars have been enigmatic since their discovery; their behavior resembles a seeping liquid but sources of water remain puzzling. This work demonstrates that the properties of RSL are consistent with observed behaviors of Martian and terrestrial aeolian processes. Specifically, RSL are well-explained as flows of sand t...
Howett, Carly Spencer, John Nordheim, Tom
We use data from Cassini's Composite Infrared Spectrometer CIRS to map Mimas' surface temperatures and its thermophysical properties. This provides a dramatic improvement on the work in Howett et al. (2011), where the values were determined at only two regions on Mimas (one inside, and another outside of the anomalous region). We use all spatially-...
Jackson, Brian
The influence of dust devils on the martian atmosphere depends on their capacity to loft dust, which depends on their wind profiles and footprint on the martian surface, i.e., on their radii, $R$. Previous work suggests the wind profile depends on a devil's thermodynamic efficiency, which scales with its height, $h$. However, the precise mechanisms...
Brossier, J.F. Gilmore, M.S. Toner, K.
Published in
Icarus
Multiple studies reveal that most of Venus highlands exhibit anomalously high radar reflectivity and low radar emissivity relative to the lowlands. This phenomenon is thought to be the result of atmosphere-surface interactions in the highlands, due to lower temperatures. These reactions are a function of rock composition, atmospheric composition, a...
Bishop, Janice L. Gross, Christoph Danielsen, Jacob Parente, Mario Murchie, Scott L. Horgan, Briony Wray, James J. Viviano, Christina Seelos, Frank P.
Published in
Icarus
Refined calibrations of CRISM images are enabling identification of smaller deposits of unique aqueous materials on Mars that reveal changing environmental conditions at the region surrounding Mawrth Vallis. Through characterization of these clay-sulfate assemblages and their association with the layered, phyllosilicate units of this region, more d...
Quillen, Alice C. Lane, Mckenzie Nakajima, Miki Wright, Esteban
Mass-spring model simulations are used to investigate past spin states of a viscoelastic Phobos and Deimos. From an initially tidally locked state, we find crossing of a spin-orbit resonance with Mars or a mean motion resonance with each other does not excite tumbling in Phobos or Deimos. However, once tumbling our simulations show that these moons...
