The predictive capability of QMD simulations allows us to determine the properties of materials subject to planetary interiors conditions. The equation-of-state (EOS) of the planetary materials, specifically the pressure as a function of density, temperature, and composition, are required in order to close the set of hydrostatic equations used in planetary models [1,2].
 D. C. Swift, J. H. Eggert, D. G. Hicks, S. Hamel, K. Caspersen, E. Schwegler, G. W. Collins, N. Nettelmann and G. J. Ackland Mass-Radius Relationships for Exoplanets. Astro. Phys. J. 744, 59 (2012)
 R. G. Kraus, S. T. Stewart, D. C. Swift, C. A. Bolme, R. F. Smith, S. Hamel, B. D. Hammel, D. K. Spaulding, D. G. Hicks, J. H. Eggert, G. W. Collins Shock vaporization of silica and the thermodynamics of planetary impact events. J. Geophys. Research – Planets 117, E09009 (2012)
 Morales, MA; Schwegler, E; Ceperley, D; Pierleoni, C; Hamel, S; Caspersen, K. Phase separation in hydrogen-helium mixtures at Mbar pressures. P. Natl. Acad. Sci. USA, 106, 1324-1329, (2009)
 S. Hamel, Miguel Morales and Eric Schwegler, Signature of helium segregation in hydrogen-helium mixtures. Phys. Rev. B 84, 165110 (2011)
 R. Chau, S. Hamel, and W. J. Nellis Chemical Processes in the Deep Interior of Uranus. Nature Communications, 2, (2011)
 M. French; S. Hamel and R. Redmer Dynamical Screening and Ionic Conductivity in Water from Ab Initio Simulations. Phys. Rev. Lett., 107, 185901 (2011)