Planetary surfaces

Abstract:

Geochemical and astronomical evidence demonstrates that planet formation occurred in two spatially and temporally separated reservoirs. The origin of this dichotomy is unknown. We use numerical models to investigate how the evolution of the solar protoplanetary disk influenced the timing of protoplanet formation and their internal evolution. Migration of the water snow line can generate two distinct bursts of planetesimal formation that sample different source regions. These reservoirs evolve in divergent geophysical modes and develop distinct volatile contents, consistent with constraints from accretion chronology, thermochemistry, and the mass divergence of inner and outer Solar System. Our simulations suggest that the compositional fractionation and isotopic dichotomy of the Solar System was initiated by the interplay between disk dynamics, heterogeneous accretion, and internal evolution of forming protoplanets.

Abstract:

Spectral data created as part of a study into the effects of aqueous and thermal alteration on the spectral signature in the NIR and MIR wavelength ranges. NIR data were collected as reflectance and MIR data were collected as emissivity under both ambient and simulated asteroid environment (SAE) conditions.

Abstract:

Data supporting the publication Transient HCl in the atmosphere of Mars in Sci. Adv. Data was created using the GGG Software Suite using measurements made with the ExoMars Trace Gas Orbiter Atmospheric Chemistry Suite.

Abstract:

Position sensitive detector X-ray diffraction (PSD-XRD) data created as part of a study into the effects of aqueous and thermal alteration on the spectral signature in the NIR and MIR wavelength ranges. Data were collected on an Enraf-Nonius PDS120 X-ray diffractometer with an INEL curved 120o PSD. Each meteorite had two diffraction patterns collected on two 50mg aliquots (HB1 and HB2) of a larger 1.8g mass powdered sample.