Radar Anomaly (Venus)
A high reflectivity radar feature concentrated in the Venusian highlands.
A type of radar feature
Strong radar signal reflected from elevations above about 2.5 km (near the equator) or 5 km (at 60°N) on Venus that becomes less pronounced at the highest elevations (Klose et al. 1992); there is also a commensurate low microwave emissivity at the same locations. The planetary average reflectivity on Venus is 0.14 ± 0.03. However, this reflectivity ranges between 0.35 ± 0.04 and 0.43 ± 0.05 in the highlands (Pettengill et al. 1988). Most of the high-altitude regions displaying anomalous reflectivity and emissivity are also very rough on centimeter to meter scales, making inference of surface properties difficult. A notable exception is the crater Cleopatra on the flank of Maxwell Montes, which has enough mirror-like surface elements that a quasi-specular echo could be measured during Magellan bistatic radar experiments in 1994.
- Kohler E, Gavin P, Chevrier V, Johnson N (2012) Experimental investigations into the radar anomalies on Venus. Lunar Planet Sci Conf XLIII, abstract #2749, The Woodlands, 19–23 MarGoogle Scholar
- Kohler E, Chevrier V, Gavin P, Johnson N (2013) Experimental stability of tellurium and its implications for the Venusian radar anomalies. Lunar Planet Sci Conf XLIV, abstract #2951, The Woodlands, 18–22 MarGoogle Scholar