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• W1550269482 abstract "Introduction: Lunar mare basalts are made up of individual, compositionally and temporally, distinct lava flows [e.g. 1, 2]. Whilst the areal extent of these flows has often been remotely mapped [e.g. 1-5], determining their thickness and volume is more problematic. There are some depth estimates for the total basalt deposits [e.g. 6-8], but there are few such estimates for the individual lava flows [e.g. 9]. In this study we use Clementine multispectral reflectance data to identify conspicuous compositional signatures associated with the continuous ejecta of impact craters within an area of Oceanus Procellarum. These ejecta represent material excavated from older lava flows beneath that in which the craters are situated; their size can therefore be used to constrain the thicknesses of the surficial flows. Methods: Clementine UV-Vis reflectance data were downloaded at full resolution (0.1 km/pixel) and in a simple cylindrical projection from the USGS MapA-Planet website (www.mapaplanet.org) as radiometrically, geometrically and photometrically controlled .raw files [10]. The files were extracted and analysed using an in-house IDL (Interactive Data Language) code. These data were used to produce maps of the study area in Oceanus Procellarum (Fig. 1) for various parameters, including FeO and TiO2 wt. % abundances (according to the algorithms of [11] and [12] respectively). Results: The TiO2 wt. % abundance map reveals a number of craters within a particular lava flow (‘P52’, as termed by [2]) that appear to be surrounded by haloes of material with a lower TiO2 content than the surrounding lava flow (see Fig. 2), and which approximate the extent of their continuous ejecta blankets (i.e. ~1 crater radius beyond the rim: [13, 14]). We hypothesize that these haloes evidence material that has been excavated from a lithology beneath the surface lava flow (‘P52’), with a lower TiO2 content. A candidate for this deeper lava flow is ‘P24’ (as termed by [2]), which is TiO2-poorer (by ~3 wt. %), and stratigraphically older than ‘P52’. Figure 3 is a plot of mean FeO and TiO2 wt. % abundances for (i) the ejecta of the thirteen craters with TiO2-poor haloes identified in lava flow ‘P52’ and (ii) the average lava flow compositions of ‘P52’ and ‘P24’. This figure illustrates that the ejecta of the thirteen haloed craters have a distinct composition from that of lava flow ‘P52’ in which they lie; the ejecta compositions are more similar to that of the proposed underlying lava flow, ‘P24’." @default.
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• W1550269482 date "2010-03-01" @default.
• W1550269482 modified "2023-09-23" @default.
• W1550269482 title "Impact Craters: Windows Through Lava Flows in Oceanus Procellarum" @default.
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