Venusian geological features and origin of the Archean Earth greenstone belts

Magellan imagery of Venus reveals a variety of geological features (e.g., coronae and impact craters) which may have been present on the early Earth and preceded the formation of Archean greenstone belts.     

Neptune's satellites: Implications from impact crater morphology

The presence of central peak craters and the absence of central pit craters on Triton implies a surface rigidity similar to the Saturnian and Uranian satellites and stronger than that of the Jupiter satellites Ganymede and Callisto. Tectonically degraded terrain may exist at the antipode of the large impact structure on 1989N1. Dome craters on Triton may represent a form of solid state volcanism.     

The prediction of aquatic sediment-associated trace element concentrations using selected geochemical factors

Multiple linear regression models calculated from readily obtainable chemical and physical parameters can explain a high percentage (70 per cent or greater) of observed sediment-trace element variance for Cu, Zn, Pb, Cr, Ni, Co, As, Sb, Se, and Hg in a widely divergent suite of 61 sediment samples. The independent variables used in the models may be single parameters, principal component scores, or principal component scores combined with their cross-products. The most useful type of variable must be determined on a case-by-case basis. The independent variables (geochemical parameters) incorporated in the models calculated during this study probably are applicable to many aquatic sediments; albeit, use of a larger data set (>61) could alter the magnitude of the calculated coefficients. The geochemical parameters included in the models were of a physical (e.g. grain size, surface area) and a chemical (e.g. organic matter, amorphous iron oxides) nature. Comparison between actual and predicted trace element concentrations obtained from the models may provide a means of defining ‘average’ sediment-trace element concentrations. In this context, the models may also help identify either naturally or anthropogenically impacted sites for additional study.     

The dayside Venus ionosphere: I. Pioneer-Venus retarding potential analyzer experimental observations

The median values of the principal ionospheric quantities of the Venus dayside ionosphere are presented. The values are derived from the quantities measured by the Pioneer-Venus orbiter retarding potential analyzer over a period of two Earth yaers at solar cycle maximum. Quantities reported are total ion density, O⁺ density, O₂⁺ density, sum density (NO⁺ + N₂⁺ + CO⁺), CO₂⁺ density, ion temperature, electron temperature, and plasma particle pressure. The data are organized to reveal altitude, solar zenith angle, solar longitude, and latitude dependences. The O⁺ density exhibits both a solar longitude and a latitude dependence which we suggest is caused by superrotation of the thermosphere and/or ionosphere. Asymmetry between the dawn and dusk terminator regions in the behavior of other quantities is also descibed.     

Volatiles,vesicles, and vugs: Unraveling the magmatic and eruptive histories of Steno crater basalts

In 1972, Apollo 17 astronauts returned 170.4 kg of lunar material. Within 1 month of their return, a subset of those samples was specially curated with the forethought that future analytical techniques would offer new insight into the formation and evolution of the Moon. Of interest in this work is sample 71036, a basalt collected from the rim of Steno crater in the Taurus–Littrow Valley, which was stored frozen and was processed and released for study 50 years later. We report, for the first time, the detailed mineralogy and petrology of 71036 and its companion samples 71035, 71037, and 71055 using a novel combination of 2-D and 3-D methods. We investigate lunar volatiles through in situ measurements of apatite and 3-D measurements of vesicles to understand the degassing histories of the Steno crater basalts. Our coupled 2-D petrography and 3-D tomography data sets support a model of the Steno crater basalts crystallizing in the upper crust of a mare lava flow. Apatite F and OH chemistry and the late-stage deformation of voids and formation of smaller vesicles provide evidence supporting coeval degassing of volatiles and crystallization of mesostasis apatite in Apollo 17 basalts. This work helps to close knowledge gaps surrounding the origin, magmatic evolution, emplacement, and crystallization history of high-titanium basalts.