Effusive Lunar Domes near Kepler and Piccolomini: Morphometry and Mode of Emplacement

Introduction: Lunar domes are smooth low features similar to low terrestrial shield volcanoes. They were formed during the terminal phases of lunar eruptions and mostly occur in the maria. A few domes have been reported in the highlands, but these are usually difficult to observe because of the brightness and ruggedness of the surrounding terrain. According to [1,2], constructional volcanic features formed during the later stages of volcanism on the Moon, characterised by a decreasing rate of lava extrusion and a comparably low eruption temperature, resulting in the formation of effusive domes. Lunar domes may also form as intrusive structures, commonly interpreted as laccoliths. In this case magma accumulates within the lunar crust, slowly increasing in pressure and causing the crustal rock above it to bow upward [2]. Recent studies about lunar domes are based on the evaluation of their spectrophotometric and morphometric properties, rheologic parameters, and their classification based on the spectra and three-dimensional shapes of the volcanic edifices [3-5]. The Consolidated Lunar Dome Catalogue [6] contains all lunar domes which have been studied in detail by the GLR group and for which accurate morphometric properties could be determined. The catalogue is continuously updated according to ongoing observing and modelling activities. In this contribution we provide an analysis of two effusive domes, located in Oceanus Procellarum to the west of the crater Kepler, and inside Rupes Altai near the crater Piccolomini, respectively.