Other
Scientific paper
Sep 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.2604c&link_type=abstract
American Astronomical Society, DPS meeting #41, #26.04
Other
Scientific paper
Lunar domes display a broad range of sizes, surface textures, and morphologies. Some domes are thought to have formed via extrusive volcanism originating from a central vent or rift, while others are thought to have formed through non-extrusive processes (Head and Gifford, Moon and Plan., 22, 235,1980). Recent high-resolution (80 m/pixel) S-band (12.6 cm wavelength) radar data obtained using Arecibo Observatory and the Green Bank Telescope can be used to investigate the surface properties of the different classes of lunar domes. The domes Manilus 1 and Mons Rümker (Carter et al., JGR, submitted, 2009; Campbell et al., JGR, 114, E01001, doi:10.1029/2008JE003253, 2009) have low circular polarization ratio values that may indicate the presence of pyroclastics. Other domes in the Mare Vaporum region have polarization characteristics that are similar to surrounding mare basalts (Carter et al. JGR, submitted, 2009). Our current radar data include areas with significant dome concentrations in the Mare Vaporum, Marius Hills, and Rimae Cauchy regions. We present preliminary results comparing the radar polarization properties of different dome types and discuss possible implications for their surface properties and evolution.
Anderson Robert F.
Campbell Bruce A.
Campbell Don B.
Carter Lynn Marie
Hawke Bernard Ray
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