Gwen Barnes (affiliate faculty)
College of Science
UI Department of Physics
Assistant Research Professor - Planetary Science
Campus Locations: Moscow
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Impact cratering on the Moon and Mars
- PhD, Planetary Science, 2007—University of Arizona, Tuscon
- BS, Chemistry, 1998—University of California, Santa Barbara
- Bart, G.D.; Nickerson, Ryan D.; Lawder, Matthew T.; Melosh, H.J. Global Survey of Lunar Regolith Depths from LROC Images. Icarus, 2011. doi:10.1016/j.icarus.2011.07.017
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Bart, G.D.; Melosh, H.J. Distributions of boulders ejected from lunar craters. Icarus, 2010, 209, 337-357. doi:10.1016/j.icarus.2010.05.023
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Bart, G.D.; Melosh, H.J. Impact Into Lunar Regolith Inhibits High Velocity Ejection of Large Blocks. J. Geophys. Res. (Planets), 2010, 115, E08004. doi:10.1029/2009JE003441.
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Bart, G.D.;Melosh, H.J. Using lunar boulders to distinguish primary from distant secondary impact craters. Geophys. Ress Lett., 2007, 34, L07203. doi:10.1029/2007GL029306
- Bart, G.D. Comparison of small lunar landslides and martian gullies. Icarus, 2007, 187, 417-421. doi:10.1016/j.icarus.2006.11.004
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Bart, G. D., E. P. Turtle, W. L. Jaeger, L. P. Keszthelyi, and R. Greenberg. Ridges and Tidal Stress on Io. Icarus, 2004, 169, 111-126. doi:10.1016/j.icarus.2004.01.003
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Greenberg, R., G. V. Hoppa, G. D. Bart, and T. A. Hurford. Tidal Stress Patterns on Europa’s Crust. Cele. Mech., 2003, 87, 171-188. doi:10.1023/A:1026169424511
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Works, C. F., C. J. Jocher, G. D. Bart, X. Bu, and P. C. Ford. Photochemical Nitric Oxide Precursors: Synthesis, Photochemistry, and Ligand Substitution Kinetics of Ruthenium Salen Nitrosyl and Ruthenium Salophen Nitrosyl Complexes. Inorganic Chemistry, 2002, 41, 3728-3739. doi: 10.1021/ic020248k
I study impact cratering on the Moon and Mars.
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My martian project is designed to understand the difference (if any) in the characteristics of ejecta from primary vs secondary craters. Primary craters are formed by a piece of interplanetary material impacting the surface at high velocities (<10 km/s or so). Secondary craters are formed by ejecta from a large crater that is traveling so fast that when it impacts the surface it also forms an impact crater. This study should have implications for understanding the ages of planetary surfaces as determined by crater counting.
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I also have a lunar project that studies a similar primary vs secondary crater problem.
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Finally, I study the depth of the lunar regolith by analyzing the size distributions of craters with specific morphologies that indicate the regolith depth.
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I also have a couple of pending projects: One is for continuing the regolith depth study; the other is for studying lunar landslide features.
