Equilibrium thermodynamics and kinetic models of graduate student Amy McAdam are used to conclude that silica rich deposits on Mars (e.g., in Gusev crater) could have formed through low-temperature acid weathering in spring locations (LPSC-2008 + paper in press in JGR-Planets)

Kinetic models of mineral dissolution developed by graduate student Amy McAdam demonstrate that preferential dissolution of pyroxene in acid fluids may explain data obtained from Mars orbiters and Mars Exploration Rovers. pdf

Physical-chemical modeling is used to evaluate oceanic composition on the Jovian icy satellite Europa. pdf

Coupled thermodynamic-kinetic modeling of water-rock interaction is used to evaluate early stages of aqueous alteration on parent bodies of carbonaceous chondrites (pdf-1, pdf-2)

Thermodynamic and kinetic models of graduate student Christopher Glein demonstrate that the composition of Enceladus plume detected by the Cassini spacecraft could be explained by hydrothermal processes on the early satellite. pdf

Equilibrium thermodynamics and mass balance constraints were used to evaluate oceanic composition on early and today's Enceladus.

Coupled thermodynamic/kinetic modeling of aqueous weathering shows that Martian surface could have been affected by short-term acid rainfalls caused by strong meteoritic impacts. A presence of silica and a deficiency of pyroxene observed in some low-albedo regions imply low-pH weathering without neutralization.

Chemical aspects of atmosphere-surface interactions on Venus and Mars have been reviewed.

Thermodynamic/kinetic modeling is used to explore fate of phyllosilicates on Mars. We show that clays are more stable than many primary and secondary minerals and could survive acid attacks.

Physical-chemical modeling is used to evaluate chemical evolution of a primordial ocean on Europa.

It is proposed that an organic layer below the ice shell on Enceladus could account for the generation of tidal heat and plume gases observed by the Cassini spacecraft during 2005 flyby.

We hypothesized that HCl hydrate formed in the solar nebula and then accreted in asteroids, planets and satellites. Performed physical-chemical analysis shows that early acid fluids in asteroids could have been present as HCl-rich aqueous solutions formed through eutectic (~186 K) melting of HCl hydrate.

Thermodynamic modeling in isochoric systems was used to evaluate pressure during aqueous processes in asteroids.