Theia Mons (centered at 23.4° N, 79.4° W) is the main volcanic center for the Beta Regio plume, of the Beta-Atla-Themis (BAT) region, Venus. Synthetic aperture radar data (SAR) and altimetry data from the 1989–1994 NASA Magellan mission were used to produce a geological map and history of Theia Mons, revealing two distinct magmatic centers (200 km apart), each the focus of basaltic lava flows, extensional lineaments (representing the surface expression of dyke swarms), and associated rift zones. The study area spans 88°W to 72°W, 16°45′N to 29°45′N, and mapping was at 1:500,000 scale. Our detailed mapping makes this area a prime target for the future Venus missions (orbital and lander), also given that Beta Regio is a strong candidate for ongoing volcanic activity. Lava (basaltic) flow units (88 distinguished on the basis of variation in radar backscatter) belonging to Theia Mons volcano were combined into 19 Flow Groups and then into 3 Flow Packages. The lava flows appear to diverge from two distinct magmatic centers, labelled Center 1 (24.5°N, 78.1°W) and Center 2 (23.4° N, 79.4°W), with the older Center 1 being obscured by the volcanism of the younger Center 2. Center 1 consists of flows with low radar brightness and which extend to a maximum to 830 km from the center. Center 2 coincides with the currently preserved central caldera and consists of lava flows of low radar brightness with a maximum length of 620 km, followed by a second pulse of radar-bright flows that are less extensive and concentrated near the center. About 10,000 extensional lineaments (grabens, fissures, and fractures) were mapped and grouped into 19 systems, of which 15 are interpreted to overlie dyke swarms: 2 radiating systems are associated with Centers 1 and 2, and 13 other systems belong to other (older and likely unrelated) magmatic centers in the region. A partial circumferential swarm may also be present, associated with Center 2. Four other extensional lineaments sets are inferred to represent sets of normal faults associated with rift zones (Devana and Zverine, and additional rift zones). These rift zones exhibit two sets of ‘triple junction’ geometry, which are approximately also focussed on the same Centers 1 and 2, revealed by the lava flows and rift zones. An underlying mantle plume is interpreted to be responsible for the dykes, flows and triple junction rifting. The cause of the shift between Centers 1 and 2 (200 km to SW) is unknown, but plausible mechanisms include a shift of the lithospheric plate above a stationary single plume, or a bending of the mantle plume (e.g. in a mantle wind) between timing of Center 1 and Center 2 activity. • Detailed mapping of flows, graben systems & rift zones of Theia Mons, Venus. • Mapping of 88 lava flows, combined into 19 flow groups and 3 flow packages. • 10,000 graben systems mapped & grouped in 19 sets-at least 15 overlie dyke swarms. • Two centers, each the focus of radial flows, dyke swarms & triple junction rifting. • The 200 km between centers due to movement between lithosphere & underlying plume.

We present a technique for improving the spatial resolution of satellite spectrophotometric data of the Moon’s surface using an artificial neural network. We demonstrate this approach using the high-spectral low-spatial resolution Moon Mineralogy Mapper (M 3 ) spectrophotometer and the low-spectral high-spatial resolution Multiband Imager (MI) Kaguya datasets for super-resolution olivine mapping over the Copernicus crater. The super-resolution of spectral maps is achieved by correlating spectral data of these instruments using a multilayer perceptron. An important advantage of the method is the use of a single data frame from each dataset to study a particular lunar region. The obtained maps of the olivine abundance provide new spatial context of the investigated mineral distribution: olivine-rich surface units become visible primarily as flow tubes, lava ponds on the crater walls and boulder outcrops associated with high olivine content (up to 90 vol.%) at the central peak of the investigated crater. The content of the olivine-reaches deposits of the area on the central peak reaches up to 35 vol. % of the lunar regolith. • A super-resolution technique is proposed for high – resolution olivine mapping • The content of lunar olivine varies from 0 to 35 vol. % for the Copernicus crater region • High-olivine spots are associated with surface areas covered with boulders • Shapes and morphology of smaller deposits on the northern slope are refined

Of the planets in our solar system, Mars may be the most likely place to find evidence of life and learn about planetary evolution. However, in exploring Mars, we risk damaging sites of possible outstanding universal geoheritage value due to a lack of legal frameworks or practical guidelines. This study sought to develop practical exogeoconservation methods and test these at the Mars Desert Research Station (MDRS) over two crew rotations, totalling one month. However, there were several unanticipated challenges both in pre-mission planning and on-site, in-person exploration, making effective, practical exogeoconservation extremely challenging. This analogue study has implications for continued Mars exploration, as without practical exogeoconservation methods, we may risk the destruction of sites of possible outstanding universal geoheritage value on Mars. We find that exogeoconservation of Mars will require significantly more detailed information and study than is currently available. A key implication of this study is that sampling of potentially important outcrops should be reserved until after a whole area has been explored in-depth, to ensure the samples taken are both exceptional and common enough to allow for their removal. We also find that there is a role for geoconservation experts on Mars exploration teams to bring exogeoconservation principles to the forefront of Mars missions. • Practical exogeoconservation methods were investigated at a Mars analogue site. • Several unforeseen challenges occurred throughout the study. • Exogeoconservation of Mars requires more detailed information than is available. • Sampling important outcrops should occur only after in-depth exploration. • There is a role for geoconservation experts on Mars exploration teams.

The DESTINY+ spacecraft will be launched to the active asteroid (3200) Phaethon in 2025. The spacecraft will be equipped with the DESTINY+ Dust Analyzer (DDA) which will be a time-of-flight impact ionization mass spectrometer. In addition to the composition of impacting dust particles, the instrument will measure the particle mass, velocity vector, and surface charge. Here, we study the detection conditions of DDA for interstellar dust during the DESTINY+ mission. We use the interstellar dust module of the Interplanetary Meteoroid environment for EXploration model (IMEX Sterken et al., 2013; Strub et al., 2019) to simulate the flow of interstellar dust through the Solar System. Extending earlier work by Krüger et al. (2019b) we consider the entire DESTINY+ mission, i.e. the Earth-orbiting phase of the spacecraft during the initial approximately 1.5 years after launch, the nominal interplanetary mission phase up to the Phaethon flyby, and a four-years mission extension beyond the Phaethon flyby. The latter may include additional asteroid flybys. For predicting dust fluxes and fluences we take into account a technical constraint for DDA not to point closer than 90° towards the Sun direction for health and safety reasons of the instrument and in order to avoid electrical noise generated by photoelectrons. For the Earth orbiting phase after launch of DESTINY+ our simulations predict that up to 28 interstellar particles will be detectable with DDA in 2026. In the following years the interplanetary magnetic field changes to a focussing configuration for small (≲0.1μm) interstellar dust particles. This increases the total number of detectable particles to 50 during the interplanetary mission of DESTINY+ in 2027. In 2028 and 2029/30 approximately 160 and 190 particles will be detectable, respectively, followed by about 500 in 2030/31. We also make predictions for the detectability of organic compounds contained in the interstellar particles which is a strong function of the particle impact speed onto the detector. While organic compounds will be measurable only in a negligible number of particles during the Earth orbiting and the nominal interplanetary mission phases, a few 10s of interstellar particle detections with measurable organic compounds are predicted for the extended mission from 2028 to 2031.