RT @theAGU: Today, we celebrate all of the incredible #WomenInScience around the world serving as Editors, Associate Editors, and #PeerRevi…

Seismic Wavefield Modeling of Enceladus: Challenges and Opportunities Presented by a 3D Ice Shell. Study recommends a landing site 20–30° from the south pole to observe a range of ice-, ocean-, and core-transmitted seismic phases.

Mapping of Western Valles Marineris Light-Toned Layered Deposits and Newly Classified Rim Deposits. Light-toned layered deposits (LLD) on the plateaus of Valles Marineris show clear basal reflections when examined using the Shallow Radar (SHARAD).

Study of an Extremely Strong Quasi-20-Sol Wave During a Global Dust Storm in Mars Year 34. The quasi-20-sol wave is mainly enhanced by a prominent temperature increase caused by a global dust storm.

Extensive Secondary Cratering From the InSight Sol 1034a Impact Event. A new 9-m-diameter impact crater on Mars is identified with in situ seismic and orbital image data; over 900 low albedo spots identified as a result of secondary ejecta processes.

Ignan Earths: Habitability of Terrestrial Planets With Extreme Internal Heating. Terrestrial planets with extreme internal heating may exhibit rheologically solid mantles, and thus stable crusts.

Characterizing the Modulation and Activation-Triggering Mechanisms of Main-Belt Comets via 3D Thermophysical Modeling of an Ellipsoidal Body. A large obliquity may play important role in enhancing detectability of sublimation-driven dust emission in MBCs

Pluto Geologic Map: Use of Crater Data to Understand Age Relationships. Young, crater-free, areas with widely varying geomorphology make up a large fraction, about 30%, of Pluto's near-side.

Using the Melosh Model of Acoustic Fluidization to Simulate Impact Crater Collapse on the Earth and Moon. Consideration of the full model of acoustic fluidization produces a variety of subsurface deformation in complex craters lacking in other models.

Impact of Solar Wind Density and Velocity Variations on the Martian Magnetosphere and Ion Escape Process. Model demonstrates that under constant dynamic pressure, a decrease in solar wind velocity leads to a stronger solar wind dynamo.

Lunar Crustal KREEP Distribution. Nearside thorium distribution is well explained by Th-enriched Imbrium ejecta impacting lower-Th crust.

Complex Crater Collapse: A Comparison of the Block and Melosh Acoustic Fluidization Models of Transient Target Weakening. Regeneration of acoustic energy facilitates localized deformation and sustains vibrations for the duration of crater collapse.

Diagenesis of the Clay-Sulfate Stratigraphic Transition, Mount Sharp Group, Gale Crater, Mars. Observed textures and their associated chemistry suggest several diagenetic episodes and concentrations of Mg sulfate in nodules and cement.

Run-Away Transition to Turbulent Strong-Field Dynamo. This work employs a data-driven analysis of subcritical transition from weak- to strong-field dynamo regimes.

Ultraviolet NO and Visible O2 Nightglow in the Mars Southern Winter Polar Region: Statistical Study and Model Comparison. The NO emitting layer is found to be consistently located ∼10 km above the O2 nightglow layer (∼55 and ∼45 km, respectively).

Martian Atmospheric Disturbances From Orbital Images and Surface Pressure at Jezero Crater, Mars, During Martian Year 36. Correlates pressure variability & oscillations with dust storms, clouds and baroclinic cyclones studied from images taken from orbit.

Simple-To-Complex Crater Transition for the Uranian Satellites Ariel and Miranda. Study finds the transition diameter for Ariel is consistent with it being differentiated, with a primarily icy surface.

Electron-Induced Radiolysis of Water Ice and the Buildup of Oxygen. Study finds that the dominant radiolysis products released from the ice samples are H2 and O2, with a fraction of the O2 being retained in the ice.

Seasonal and Inter-Annual Variability in the Polar Vortex and Snowfall on Mars. Study finds that the shape, size, and stability of the Martian polar vortices are controlled by topography, dust loading, and insolation.

Clouds and Ammonia in the Atmospheres of Jupiter and Saturn Determined From a Band-Depth Analysis of VLT/MUSE Observations. Band-depth approximation analysis from 600 to 680 nm reliably maps NH3 abundance at 2–3 bars in atmospheres of Jupiter and Saturn.