A5004071446- Planetary Science and Exploration
- Astro and Planetary Science
- Space Exploration and Technology
- Cryospheric studies and observations
- Space Science and Extraterrestrial Life
- Arctic and Antarctic ice dynamics
- Geology and Paleoclimatology Research
- Methane Hydrates and Related Phenomena
- Spacecraft and Cryogenic Technologies
- Spaceflight effects on biology
- Isotope Analysis in Ecology
- Space Satellite Systems and Control
- Geophysics and Gravity Measurements
- Academic Publishing and Open Access
- Scientific Research and Discoveries
- Spacecraft Design and Technology
- Geomagnetism and Paleomagnetism Studies
- Landslides and related hazards
- Winter Sports Injuries and Performance
- Geotourism and Geoheritage Conservation
- GNSS positioning and interference
- Religious Studies and Spiritual Practices
- Spacecraft Dynamics and Control
- Hydrocarbon exploration and reservoir analysis
- Time Series Analysis and Forecasting
Purdue University West Lafayette
2020-2025
University of Arizona
2015-2021
Macau University of Science and Technology
2021
University of Aberdeen
2021
Lunar and Planetary Institute
2018-2020
Planetary Science Institute
2017-2019
Water ice cliffs on Mars Some locations are known to have water just below the surface, but how much has remained unclear. Dundas et al. used data from two orbiting spacecraft examine eight where erosion occurred. This revealed composed mostly of ice, which is slowly sublimating as it exposed atmosphere. The sheets extend surface a depth 100 meters or more and appear contain distinct layers, could preserve record Mars' past climate. They might even be useful source for future human...
Abstract Troughs carved into Mars' polar ice cap expose layers of different brightness and topography. These can be divided two strata types: darker, higher dust content marker beds brighter, lower interbeds. In a companion paper (Pascuzzo et al., 2025, https://doi.org/10.1029/2024JE008377 ), we measure the topographic protrusion Here, investigate processes factors that contribute to evolution these gain insight sublimation rates timescales for active trough wall retreat, specifically...
Abstract Although ice in the Martian midlatitudes is typically covered by a layer of dust or regolith, it exposed some locations fresh impact craters erosional scarps. In both cases, massive excess with low lithic content. We find that scarps occur between 50° and 61° north south latitude they are concentrated near Milankovič crater northern hemisphere southeast Hellas basin southern hemisphere. These may represent particularly thick clean bodies ice. Pits created retreat...
Abstract The Miniature Radio Frequency instrument (Mini-RF) on the Lunar Reconnaissance Orbiter obtained widespread synthetic aperture radar observations of Moon in S band (12.6 cm), including nearly complete coverage at both lunar poles. currently archived monostatic data have spatial offsets from reference frame, making them more difficult to compare other sets. To address this issue, we developed a new algorithm for spatially controlling Mini-RF S-band set and orthorectifying these onto...
Abstract Mars' north polar ice cap features troughs that cut into the ice, exposing subsurface layers of different brightness and topographic expression. Specifically, these represent two stratum types: lower albedo (higher dust content) marker beds, which protrude out wall topographically, higher (i.e., icier) interbeds, are recessed compared to beds. Here, we investigate role local‐scale processes by performing a detailed geomorphic characterization variability in strata across sites,...
The distribution of subsurface water ice on Mars is a key constraint past climate, while the volumetric concentration buried (pore-filling versus excess) provides information about process that led to its deposition. We investigate Arcadia Planitia by measuring depth terraces in simple impact craters and mapping widespread reflection radar sounding data. Assuming contrast material strengths responsible for terracing same dielectric interface causes reflection, we can combine these data...
Abstract Recent analysis of radar data from the Mars Express spacecraft has interpreted bright subsurface reflections as indicators local liquid water at base south polar layered deposits (SPLD). However, physical and geological conditions required to produce melting this location were not quantified. Here we use thermophysical models constrain parameters necessary generate beneath SPLD. We show that no concentration salt is sufficient melt ice SPLD in present day under typical Martian...
Abstract Excess ice with a minimum age of tens millions years is widespread in Arcadia Planitia on Mars, and similar deposit has been found Utopia Planitia. The conditions that led to the formation preservation these midlatitude sheets hold clues past climate subsurface structure Mars. We simulate thermal stability retreat buried excess over 21 Myr Martian orbital solutions find can be orders magnitude older than obliquity cycles are typically thought drive deposition sublimation. Retreat...
Abstract Ahuna Mons is a 4 km tall mountain on Ceres interpreted as geologically young cryovolcanic dome. Other possible features are more ambiguous, implying that cryovolcanism only recent phenomenon or other structures have been modified beyond easy identification. We test the hypothesis Cerean domes viscously relax, precluding ancient from recognition. use numerical models to predict flow velocities of be 10–500 m/Myr, depending upon assumptions about ice content, rheology, grain size,...
A main goal of human space exploration is to develop humanity into a multi-planet species where civilization extends beyond planet Earth. Establishing self-sustaining presence on Mars key achieving this goal. In situ resource utilization (ISRU) critical component enabling humans both establish long-term outposts and become self-reliant. This article focuses mission architecture using the SpaceX Starship as cargo crew vehicles for journey Mars. The first Starships flown will be uncrewed...
Abstract Water ice in the Martian mid‐latitudes has advanced and retreated response to variations planet's orbit, obliquity, climate. A 150 m‐diameter new impact crater near 35°N provides lowest‐latitude exposure of subsurface on Mars. This is largest known ice‐exposing key constraints climate history. indicates a regional, relatively pure deposit that unstable nearly vanished. In past, this may have been tens meters thick extended equatorward 35°N. We infer it overlain by pore emplaced...
Abstract Mars has an extensive yet poorly understood cryosphere. Nevertheless, both direct and indirect evidence indicates buried ice across the midlatitudes, including locations where it is presently unstable. While much progress been made in exploring processes responsible for deposition preservation during recent climatic fluctuations, a global assessment of multiple reservoirs remains elusive. Motivated by science need to find suitable human landing sites, Subsurface Water Ice Mapping...
NASA’s Mini-RF instrument on the Lunar Reconnaissance Orbiter (LRO) is a hybrid-polarized, dual-frequency synthetic aperture radar (SAR) that operates at S- (12.6 cm) and X/C-band (4.2 . initially operated as monostatic system – i.e., antenna transmitter receiver co-located. A anomaly led to transitioning bistatic architecture transmitting from Arecibo Observatory (AO) or Goldstone deep space communications complex DSS-13 receiving LRO spacecraft. These data can be used...
Abstract Measurements of the lunar surface have revealed a variable presence hydration, which has contributions from both hydroxyl (OH) and molecular water (H 2 O). Recent observations hydration suggest that component this signature is comprised molecules are readily mobile actively migrate across over course day due to temperature variations. However, exospheric measurements H O very low abundances above dayside previous work argued in conflict with putative occurance ballistic migration....
Abstract The 27 satellites of Uranus are enigmatic, with dark surfaces coated by material that could be rich in organics. Voyager 2 imaged the southern hemispheres Uranus’s five largest “classical” moons—Miranda, Ariel, Umbriel, Titania, and Oberon, as well ring moon, Puck—but their northern were largely unobservable at time flyby not imaged. Additionally, no spatially resolved data sets exist for other 21 known moons, surface properties essentially unknown. Because was equipped a...
Abstract Wrinkle ridges are the predominant tectonic structure on nearside lunar maria. Although wrinkle ridge formation began as early ∼3.9–4.0 Ga, recent investigations have identified in maria that were tectonically active recently Copernican period of geologic history. Some those geologically young by presence dense fields meter-scale boulders their scarps and topographic crests. Other lack ubiquitous boulder fields, thereby rendering ambiguous search for ongoing activity Moon. Here we...
Abstract Hrad Vallis is an Amazonian‐age outflow channel located in the northwestern part of Elysium Volcanic Province Mars. The formation may have been associated with catastrophic aqueous floods and volcanism, which makes determining its emplacement history important for constraining planet's hydrological thermal evolution during Amazonian Period. Through geological mapping, geomorphologic analysis, numerical simulations we assess whether formed association mudflows (i.e., lahars),...
Abstract Mars' iconic polar spiral troughs are 400–1,000‐m‐deep depressions in the north layered deposits. As deposits accumulate, migrate approximately poleward, anti‐parallel to local wind patterns. Insolation is suspected drive ice retreat through sublimation. Sublimation at trough wall produces a growing sublimation lag that modulates further retreat; however, winds move material off retreating slope faces, thinning lag. Discontinuities stratigraphy seen by radar highlight Trough...