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xmlns="http://www.w3.org/2000/svg" viewBox="0 0 320 512"><path d="M137.4 374.6c12.5 12.5 32.8 12.5 45.3 0l128-128c9.2-9.2 11.9-22.9 6.9-34.9s-16.6-19.8-29.6-19.8L32 192c-12.9 0-24.6 7.8-29.6 19.8s-2.2 25.7 6.9 34.9l128 128z"/></svg>Most read</button></h2><div class="reveal-content tabpanel__content" style="display: none"><p><button data-reveal-label-alt="Close all abstracts" class="reveal-all-trigger mr-2 small" data-reveal-text="Open all abstracts" data-link-purpose-append="in this tab" data-link-purpose-append-open="in this tab"> Open all abstracts<span class="offscreen-hidden">, in this tab</span></button></p><div class="art-list"><div class="art-list-item reveal-container reveal-closed"><div class="art-list-item-body"><div class="eyebrow"><span class="offscreen-hidden">The following article is </span><span class="red">Open access</span></div><a href="/article/10.3847/PSJ/ad9eaa" class="art-list-item-title event_main-link">Recent Tectonic Deformation of the Lunar Farside Mare and South Pole–Aitken Basin</a><p class="small art-list-item-meta">C. A. Nypaver <em>et al</em> 2025 <em>Planet. Sci. J.</em> <b>6</b> 16 </p><div class="art-list-item-tools small wd-abstr-upper"><button type="button" class="reveal-trigger mr-2 nowrap"><svg aria-hidden="true" class="fa-icon fa-icon--left fa-icon--flip" role="img" focusable="false" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 320 512"><path d="M137.4 374.6c12.5 12.5 32.8 12.5 45.3 0l128-128c9.2-9.2 11.9-22.9 6.9-34.9s-16.6-19.8-29.6-19.8L32 192c-12.9 0-24.6 7.8-29.6 19.8s-2.2 25.7 6.9 34.9l128 128z"/></svg><span class="reveal-trigger-label" data-reveal-text="Open abstract" data-reveal-label-alt="Close abstract" data-link-purpose-append="Recent Tectonic Deformation of the Lunar Farside Mare and South Pole–Aitken Basin" data-link-purpose-append-open="Recent Tectonic Deformation of the Lunar Farside Mare and South Pole–Aitken Basin">Open abstract</span></button><a href="/article/10.3847/PSJ/ad9eaa/meta" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="View article"><span class="icon-article"></span>View article<span class="offscreen-hidden">, Recent Tectonic Deformation of the Lunar Farside Mare and South Pole–Aitken Basin</span></a><a href="/article/10.3847/PSJ/ad9eaa/pdf" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="PDF"><span class="icon-file-pdf"></span>PDF<span class="offscreen-hidden">, Recent Tectonic Deformation of the Lunar Farside Mare and South Pole–Aitken Basin</span></a><a href="/article/10.3847/PSJ/ad9eaa/epub" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="ePub"><span class="icon-epub"></span><span class="offscreen-hidden">Download </span>ePub<span class="offscreen-hidden">, Recent Tectonic Deformation of the Lunar Farside Mare and South Pole–Aitken Basin</span></a></div><div class="reveal-content"><div class="article-text view-text-small"><p>The timing and scale of lunar tectonism provide a crucial insight into the geologic evolution of Earth's Moon. Within the nearside lunar maria, wrinkle ridges formed during and after the emplacement of the mare basalts as a result of subsidence-induced contraction. Past analyses of lunar wrinkle ridges and associated fault structures have helped to constrain lunar tectonic and thermal history. However, contractional tectonics in the lunar maria may not be limited to the formation of large-scale structures in the distant geologic past. In contrast to larger, subsidence-induced lunar wrinkle ridges, recent investigations have identified contractional structures within the nearside lunar maria that are dimensionally small and recently formed via a combination of global stresses. The identification of those small mare ridges (SMRs) demonstrated that the lunar nearside maria are subject to compressional stresses that are recently and potentially currently active, but the presence of such features in the lunar farside maria was never investigated. Furthermore, the exact timing of SMR formation and the geometry of the associated fault structures remain poorly constrained. Here, we present the first observations of widespread SMRs in the lunar farside maria and South Pole–Aitken Basin. We also derive absolute model age estimates for SMR formation, and we constrain SMR-forming fault geometries via elastic dislocation modeling. Our analysis provides the first globally complete perspective of recent lunar tectonics, and we show that lunar fault structures may be recently and potentially currently active within regions of interest for upcoming lunar missions.</p></div><div class="art-list-item-tools small wd-abstr-lower"><a class="mr-2" href="https://doi.org/10.3847/PSJ/ad9eaa">https://doi.org/10.3847/PSJ/ad9eaa</a></div></div></div></div><div class="art-list-item reveal-container reveal-closed"><div class="art-list-item-body"><div class="eyebrow"><span class="offscreen-hidden">The following article is </span><span class="red">Open access</span></div><a href="/article/10.3847/PSJ/ad9824" class="art-list-item-title event_main-link">Nongravitational Forces in Planetary Systems</a><p class="small art-list-item-meta">David Jewitt 2025 <em>Planet. Sci. J.</em> <b>6</b> 12 </p><div class="art-list-item-tools small wd-abstr-upper"><button type="button" class="reveal-trigger mr-2 nowrap"><svg aria-hidden="true" class="fa-icon fa-icon--left fa-icon--flip" role="img" focusable="false" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 320 512"><path d="M137.4 374.6c12.5 12.5 32.8 12.5 45.3 0l128-128c9.2-9.2 11.9-22.9 6.9-34.9s-16.6-19.8-29.6-19.8L32 192c-12.9 0-24.6 7.8-29.6 19.8s-2.2 25.7 6.9 34.9l128 128z"/></svg><span class="reveal-trigger-label" data-reveal-text="Open abstract" data-reveal-label-alt="Close abstract" data-link-purpose-append="Nongravitational Forces in Planetary Systems" data-link-purpose-append-open="Nongravitational Forces in Planetary Systems">Open abstract</span></button><a href="/article/10.3847/PSJ/ad9824/meta" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="View article"><span class="icon-article"></span>View article<span class="offscreen-hidden">, Nongravitational Forces in Planetary Systems</span></a><a href="/article/10.3847/PSJ/ad9824/pdf" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="PDF"><span class="icon-file-pdf"></span>PDF<span class="offscreen-hidden">, Nongravitational Forces in Planetary Systems</span></a><a href="/article/10.3847/PSJ/ad9824/epub" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="ePub"><span class="icon-epub"></span><span class="offscreen-hidden">Download </span>ePub<span class="offscreen-hidden">, Nongravitational Forces in Planetary Systems</span></a></div><div class="reveal-content"><div class="article-text view-text-small"><p>Nongravitational forces play surprising and, sometimes, centrally important roles in shaping the motions and properties of small planetary bodies. In the solar system, the morphologies of comets, the delivery of meteorites, and the shapes and dynamics of asteroids and binaries are all affected by nongravitational forces. In exoplanetary systems and debris disks, nongravitational forces affect the lifetimes of circumstellar particles and feed refractory debris to the photospheres of the central stars. Unlike the gravitational force, which is a simple function of the well-known separations and masses of bodies, the nongravitational forces are frequently functions of poorly known or even unmeasurable physical properties. Here, we present order-of-magnitude descriptions of nongravitational forces, with examples of their application.</p></div><div class="art-list-item-tools small wd-abstr-lower"><a class="mr-2" href="https://doi.org/10.3847/PSJ/ad9824">https://doi.org/10.3847/PSJ/ad9824</a></div></div></div></div><div class="art-list-item reveal-container reveal-closed"><div class="art-list-item-body"><div class="eyebrow"><span class="offscreen-hidden">The following article is </span><span class="red">Open access</span></div><a href="/article/10.3847/PSJ/ad8b41" class="art-list-item-title event_main-link">Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity</a><p class="small art-list-item-meta">Brian Jackson <em>et al</em> 2025 <em>Planet. Sci. J.</em> <b>6</b> 21 </p><div class="art-list-item-tools small wd-abstr-upper"><button type="button" class="reveal-trigger mr-2 nowrap"><svg aria-hidden="true" class="fa-icon fa-icon--left fa-icon--flip" role="img" focusable="false" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 320 512"><path d="M137.4 374.6c12.5 12.5 32.8 12.5 45.3 0l128-128c9.2-9.2 11.9-22.9 6.9-34.9s-16.6-19.8-29.6-19.8L32 192c-12.9 0-24.6 7.8-29.6 19.8s-2.2 25.7 6.9 34.9l128 128z"/></svg><span class="reveal-trigger-label" data-reveal-text="Open abstract" data-reveal-label-alt="Close abstract" data-link-purpose-append="Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity" data-link-purpose-append-open="Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity">Open abstract</span></button><a href="/article/10.3847/PSJ/ad8b41/meta" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="View article"><span class="icon-article"></span>View article<span class="offscreen-hidden">, Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity</span></a><a href="/article/10.3847/PSJ/ad8b41/pdf" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="PDF"><span class="icon-file-pdf"></span>PDF<span class="offscreen-hidden">, Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity</span></a><a href="/article/10.3847/PSJ/ad8b41/epub" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="ePub"><span class="icon-epub"></span><span class="offscreen-hidden">Download </span>ePub<span class="offscreen-hidden">, Profiling Near-surface Winds on Mars Using Attitude Data from Mars 2020 Ingenuity</span></a></div><div class="reveal-content"><div class="article-text view-text-small"><p>We used attitude data from the Mars Ingenuity helicopter with a simple steady-state model to estimate wind speeds and directions at altitudes between 3 and 24 m, the first time winds at such altitudes have been probed on Mars. We compared our estimates to wind data from the meteorology package MEDA on board the Mars 2020 Perseverance rover and to predictions from meteorological models. Wind directions inferred from Ingenuity data agreed with the directions measured by MEDA, when the latter were available, but deviated from model-predicted directions by as much as 180° in some cases. The inferred wind speeds are often much higher than expected. For example, meteorological predictions suggest that Ingenuity should not have seen wind speeds above about 15 m s<sup>−1</sup> during its 59th flight, but we inferred speeds reaching nearly 25 m s<sup>−1</sup>. For flights during which we have MEDA data to compare to, inferred wind speeds imply friction velocities >1 m s<sup>−1</sup> and roughness lengths >10 cm, which seem implausibly large. These results suggest that Ingenuity was probing winds sensitive to aerodynamic conditions hundreds of meters upwind instead of the conditions very near Mars 2020, but they may also reflect a need for updated boundary layer wind models. An improved model for Ingenuity's aerodynamic response that includes the effects of transient winds may also modify our results. In any case, the work here provides a foundation for exploration of planetary boundary layers using drones and suggests important future avenues for research and development.</p></div><div class="art-list-item-tools small wd-abstr-lower"><a class="mr-2" href="https://doi.org/10.3847/PSJ/ad8b41">https://doi.org/10.3847/PSJ/ad8b41</a></div></div></div></div><div class="art-list-item reveal-container reveal-closed"><div class="art-list-item-body"><div class="eyebrow"><span class="offscreen-hidden">The following article is </span><span class="red">Open access</span></div><a href="/article/10.3847/PSJ/ad9d3f" class="art-list-item-title event_main-link">Ariel's Medial Grooves: Spreading Centers on a Candidate Ocean World</a><p class="small art-list-item-meta">Chloe B. Beddingfield <em>et al</em> 2025 <em>Planet. Sci. J.</em> <b>6</b> 32 </p><div class="art-list-item-tools small wd-abstr-upper"><button type="button" class="reveal-trigger mr-2 nowrap"><svg aria-hidden="true" class="fa-icon fa-icon--left fa-icon--flip" role="img" focusable="false" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 320 512"><path d="M137.4 374.6c12.5 12.5 32.8 12.5 45.3 0l128-128c9.2-9.2 11.9-22.9 6.9-34.9s-16.6-19.8-29.6-19.8L32 192c-12.9 0-24.6 7.8-29.6 19.8s-2.2 25.7 6.9 34.9l128 128z"/></svg><span class="reveal-trigger-label" data-reveal-text="Open abstract" data-reveal-label-alt="Close abstract" data-link-purpose-append="Ariel’s Medial Grooves: Spreading Centers on a Candidate Ocean World" data-link-purpose-append-open="Ariel’s Medial Grooves: Spreading Centers on a Candidate Ocean World">Open abstract</span></button><a href="/article/10.3847/PSJ/ad9d3f/meta" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="View article"><span class="icon-article"></span>View article<span class="offscreen-hidden">, Ariel's Medial Grooves: Spreading Centers on a Candidate Ocean World</span></a><a href="/article/10.3847/PSJ/ad9d3f/pdf" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="PDF"><span class="icon-file-pdf"></span>PDF<span class="offscreen-hidden">, Ariel's Medial Grooves: Spreading Centers on a Candidate Ocean World</span></a><a href="/article/10.3847/PSJ/ad9d3f/epub" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="ePub"><span class="icon-epub"></span><span class="offscreen-hidden">Download </span>ePub<span class="offscreen-hidden">, Ariel's Medial Grooves: Spreading Centers on a Candidate Ocean World</span></a></div><div class="reveal-content"><div class="article-text view-text-small"><p>We present evidence that Ariel's massive chasma-medial groove systems formed via spreading, where internally sourced material ascended and formed new crust. Evidence for this interpretation includes close alignment of offset faults and chasma margins during reconstruction, axial troughs bounded by raised rims, bowed-up chasma floors with marginal valleys, subparallel chasma floor ridges, and relatively young medial groove–bounding terrain. Ariel's medial grooves are among the youngest known Uranian moon geologic features and might be conduits to the interior and the source of NH-bearing species, CO, CO<sub>2</sub>, and other potential internally derived volatiles detected on the surface. While medial grooves are observable in Brownie and Kewpie Chasmata, our results indicate that these features are also present below Voyager 2 Imaging Science System image resolutions in Korrigan, Pixie, and Sylph Chasmata. Close flybys of Ariel with a Uranus orbiter are imperative to uncover the nature of these curious features and to gain insight into this moon's most recent geologic events.</p></div><div class="art-list-item-tools small wd-abstr-lower"><a class="mr-2" href="https://doi.org/10.3847/PSJ/ad9d3f">https://doi.org/10.3847/PSJ/ad9d3f</a></div></div></div></div><div class="art-list-item reveal-container reveal-closed"><div class="art-list-item-body"><div class="eyebrow"><span class="offscreen-hidden">The following article is </span><span class="red">Open access</span></div><a href="/article/10.3847/PSJ/ad9de1" class="art-list-item-title event_main-link">Impact of Jupiter's Heating and Self-shadowing on the Jovian Circumplanetary Disk Structure</a><p class="small art-list-item-meta">Antoine Schneeberger and Olivier Mousis 2025 <em>Planet. Sci. J.</em> <b>6</b> 23 </p><div class="art-list-item-tools small wd-abstr-upper"><button type="button" class="reveal-trigger mr-2 nowrap"><svg aria-hidden="true" class="fa-icon fa-icon--left fa-icon--flip" role="img" focusable="false" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 320 512"><path d="M137.4 374.6c12.5 12.5 32.8 12.5 45.3 0l128-128c9.2-9.2 11.9-22.9 6.9-34.9s-16.6-19.8-29.6-19.8L32 192c-12.9 0-24.6 7.8-29.6 19.8s-2.2 25.7 6.9 34.9l128 128z"/></svg><span class="reveal-trigger-label" data-reveal-text="Open abstract" data-reveal-label-alt="Close abstract" data-link-purpose-append="Impact of Jupiter’s Heating and Self-shadowing on the Jovian Circumplanetary Disk Structure" data-link-purpose-append-open="Impact of Jupiter’s Heating and Self-shadowing on the Jovian Circumplanetary Disk Structure">Open abstract</span></button><a href="/article/10.3847/PSJ/ad9de1/meta" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="View article"><span class="icon-article"></span>View article<span class="offscreen-hidden">, Impact of Jupiter's Heating and Self-shadowing on the Jovian Circumplanetary Disk Structure</span></a><a href="/article/10.3847/PSJ/ad9de1/pdf" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="PDF"><span class="icon-file-pdf"></span>PDF<span class="offscreen-hidden">, Impact of Jupiter's Heating and Self-shadowing on the Jovian Circumplanetary Disk Structure</span></a><a href="/article/10.3847/PSJ/ad9de1/epub" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="ePub"><span class="icon-epub"></span><span class="offscreen-hidden">Download </span>ePub<span class="offscreen-hidden">, Impact of Jupiter's Heating and Self-shadowing on the Jovian Circumplanetary Disk Structure</span></a></div><div class="reveal-content"><div class="article-text view-text-small"><p>Deciphering the structure of the circumplanetary disk (CPD) that surrounded Jupiter at the end of its formation is key to understanding how the Galilean moons formed. Three-dimensional hydrodynamic simulations have shown that this disk was optically thick and significantly heated to very high temperatures owing to the intense radiation emitted by the hot, young planet. Analyzing the impact of Jupiter's radiative heating and shadowing on the structure of the CPD can provide valuable insights into the conditions that shaped the formation of the Galilean moons. To assess the impact of Jupiter's radiative heating and shadowing, we have developed a two-dimensional quasi-stationary CPD model and used a gray atmosphere radiative transfer method to determine the thermal structure of the disk. We find that the CPD self-shadowing has a significant effect, with a temperature drop of approximately 100 K in the shadowed zone compared to the surrounding areas. This shadowed zone, located around 10 Jupiter radii, can act as a cold trap for volatile species such as NH<sub>3</sub>, CO<sub>2</sub>, and H<sub>2</sub>S. The existence of these shadows in Jupiter's CPD may have influenced the composition of the building blocks of the Galilean moons, potentially shaping their formation and characteristics. Our study suggests that the thermal structure of Jupiter's CPD, particularly the presence of cold traps due to self-shadowing, may have played a crucial role in the formation and composition of the Galilean moons.</p></div><div class="art-list-item-tools small wd-abstr-lower"><a class="mr-2" href="https://doi.org/10.3847/PSJ/ad9de1">https://doi.org/10.3847/PSJ/ad9de1</a></div></div></div></div><div class="art-list-item reveal-container reveal-closed"><div class="art-list-item-body"><div class="eyebrow"><span class="offscreen-hidden">The following article is </span><span class="red">Open access</span></div><a href="/article/10.3847/PSJ/ad9927" class="art-list-item-title event_main-link">The Peregrine Ion Trap Mass Spectrometer (PITMS): Results from a CLPS-delivered Mass Spectrometer</a><p class="small art-list-item-meta">Barbara A. Cohen <em>et al</em> 2025 <em>Planet. Sci. J.</em> <b>6</b> 14 </p><div class="art-list-item-tools small wd-abstr-upper"><button type="button" class="reveal-trigger mr-2 nowrap"><svg aria-hidden="true" class="fa-icon fa-icon--left fa-icon--flip" role="img" focusable="false" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 320 512"><path d="M137.4 374.6c12.5 12.5 32.8 12.5 45.3 0l128-128c9.2-9.2 11.9-22.9 6.9-34.9s-16.6-19.8-29.6-19.8L32 192c-12.9 0-24.6 7.8-29.6 19.8s-2.2 25.7 6.9 34.9l128 128z"/></svg><span class="reveal-trigger-label" data-reveal-text="Open abstract" data-reveal-label-alt="Close abstract" data-link-purpose-append="The Peregrine Ion Trap Mass Spectrometer (PITMS): Results from a CLPS-delivered Mass Spectrometer" data-link-purpose-append-open="The Peregrine Ion Trap Mass Spectrometer (PITMS): Results from a CLPS-delivered Mass Spectrometer">Open abstract</span></button><a href="/article/10.3847/PSJ/ad9927/meta" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="View article"><span class="icon-article"></span>View article<span class="offscreen-hidden">, The Peregrine Ion Trap Mass Spectrometer (PITMS): Results from a CLPS-delivered Mass Spectrometer</span></a><a href="/article/10.3847/PSJ/ad9927/pdf" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="PDF"><span class="icon-file-pdf"></span>PDF<span class="offscreen-hidden">, The Peregrine Ion Trap Mass Spectrometer (PITMS): Results from a CLPS-delivered Mass Spectrometer</span></a><a href="/article/10.3847/PSJ/ad9927/epub" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="ePub"><span class="icon-epub"></span><span class="offscreen-hidden">Download </span>ePub<span class="offscreen-hidden">, The Peregrine Ion Trap Mass Spectrometer (PITMS): Results from a CLPS-delivered Mass Spectrometer</span></a></div><div class="reveal-content"><div class="article-text view-text-small"><p>The Peregrine Ion Trap Mass Spectrometer (PITMS) was a mass spectrometer designed to measure lunar gases. PITMS flew on the first flight of Astrobotic's Peregrine lander via the Commercial Lunar Payload Services (CLPS) program in 2024 January. After launch, the lander suffered a propulsion system anomaly that prevented the mission from reaching the Moon, but PITMS collected 80 high-quality spectra while in cislunar space. PITMS observed abundant outgassing products from the Peregrine lander, including water, MON-25 oxidizer from the propulsion system leak, and traces of combustion products. PITMS data help constrain the nature of the propulsion system failure: oxidizer molecular ratios show that the leak released molecules rapidly enough for them to fully dissociate, and the high observed abundances imply that the oxidizer traveled within the lander surfaces rather than jetting into space. The amount of water offgassed by the spacecraft is substantially more than other planetary spacecraft, so the PITMS results suggest that instruments flying in the CLPS paradigm need to consider lander cleanliness. Though not successful in measuring the native lunar exosphere, the PITMS results showcase the capabilities of a mass spectrometer on board a lunar lander, along with lessons in pragmatism and flexibility that would enable such an instrument to ultimately be successful in the CLPS initiative.</p></div><div class="art-list-item-tools small wd-abstr-lower"><a class="mr-2" href="https://doi.org/10.3847/PSJ/ad9927">https://doi.org/10.3847/PSJ/ad9927</a></div></div></div></div><div class="art-list-item reveal-container reveal-closed"><div class="art-list-item-body"><div class="eyebrow"><span class="offscreen-hidden">The following article is </span><span class="red">Open access</span></div><a href="/article/10.3847/PSJ/ad944d" class="art-list-item-title event_main-link">Dimorphos's Material Properties and Estimates of Crater Size from the DART Impact</a><p class="small art-list-item-meta">Angela M. Stickle <em>et al</em> 2025 <em>Planet. Sci. J.</em> <b>6</b> 38 </p><div class="art-list-item-tools small wd-abstr-upper"><button type="button" class="reveal-trigger mr-2 nowrap"><svg aria-hidden="true" class="fa-icon fa-icon--left fa-icon--flip" role="img" focusable="false" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 320 512"><path d="M137.4 374.6c12.5 12.5 32.8 12.5 45.3 0l128-128c9.2-9.2 11.9-22.9 6.9-34.9s-16.6-19.8-29.6-19.8L32 192c-12.9 0-24.6 7.8-29.6 19.8s-2.2 25.7 6.9 34.9l128 128z"/></svg><span class="reveal-trigger-label" data-reveal-text="Open abstract" data-reveal-label-alt="Close abstract" data-link-purpose-append="Dimorphos’s Material Properties and Estimates of Crater Size from the DART Impact" data-link-purpose-append-open="Dimorphos’s Material Properties and Estimates of Crater Size from the DART Impact">Open abstract</span></button><a href="/article/10.3847/PSJ/ad944d/meta" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="View article"><span class="icon-article"></span>View article<span class="offscreen-hidden">, Dimorphos's Material Properties and Estimates of Crater Size from the DART Impact</span></a><a href="/article/10.3847/PSJ/ad944d/pdf" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="PDF"><span class="icon-file-pdf"></span>PDF<span class="offscreen-hidden">, Dimorphos's Material Properties and Estimates of Crater Size from the DART Impact</span></a><a href="/article/10.3847/PSJ/ad944d/epub" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="ePub"><span class="icon-epub"></span><span class="offscreen-hidden">Download </span>ePub<span class="offscreen-hidden">, Dimorphos's Material Properties and Estimates of Crater Size from the DART Impact</span></a></div><div class="reveal-content"><div class="article-text view-text-small"><p>On 2022 September 26, the Double Asteroid Redirection Test (DART) spacecraft intentionally collided with Dimorphos, the moon of the binary asteroid system 65803 Didymos. This collision provided the first full-scale test of a kinetic impactor for planetary defense. Images from DART's DRACO camera revealed Dimorphos to be an oblate spheroid covered in boulders of varying sizes and shapes. Very little was known about Dimorphos prior to DART's impact, including its shape, structure, and material properties. Approach observations and those following the DART impact have provided crucial knowledge that narrows the parameter space relevant to modeling the impact into Dimorphos. Here we present the results of a suite of hydrocode simulations of the DART impact on Dimorphos. Despite remaining uncertainties, initial models of DART's kinetic impact provide important information about the results of DART (e.g., potential crater size and morphology, ejecta mass) and the properties of Dimorphos. Simulations here suggest that Dimorphos has near-surface strength ranging from a few Pascals to tens of kPa, which corresponds to crater sizes of ∼40–60 m. Simulated crater sizes provide a crucial comparison metric for the European Space Agency Hera mission when it arrives at the Didymos system. Hera's measurement of crater size in combination with measurement of Dimorphos's mass will allow us to assess our simulations and provide the information needed to make the DART impact experiment both the first test of a planetary defense mitigation mission and the first full-scale planetary defense simulation validation exercise.</p></div><div class="art-list-item-tools small wd-abstr-lower"><a class="mr-2" href="https://doi.org/10.3847/PSJ/ad944d">https://doi.org/10.3847/PSJ/ad944d</a></div></div></div></div><div class="art-list-item reveal-container reveal-closed"><div class="art-list-item-body"><div class="eyebrow"><span class="offscreen-hidden">The following article is </span><span class="red">Open access</span></div><a href="/article/10.3847/PSJ/ad9b24" class="art-list-item-title event_main-link">Refined Mapping of Subsurface Water Ice on Mars to Support Future Missions</a><p class="small art-list-item-meta">G. A. Morgan <em>et al</em> 2025 <em>Planet. Sci. J.</em> <b>6</b> 29 </p><div class="art-list-item-tools small wd-abstr-upper"><button type="button" class="reveal-trigger mr-2 nowrap"><svg aria-hidden="true" class="fa-icon fa-icon--left fa-icon--flip" role="img" focusable="false" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 320 512"><path d="M137.4 374.6c12.5 12.5 32.8 12.5 45.3 0l128-128c9.2-9.2 11.9-22.9 6.9-34.9s-16.6-19.8-29.6-19.8L32 192c-12.9 0-24.6 7.8-29.6 19.8s-2.2 25.7 6.9 34.9l128 128z"/></svg><span class="reveal-trigger-label" data-reveal-text="Open abstract" data-reveal-label-alt="Close abstract" data-link-purpose-append="Refined Mapping of Subsurface Water Ice on Mars to Support Future Missions" data-link-purpose-append-open="Refined Mapping of Subsurface Water Ice on Mars to Support Future Missions">Open abstract</span></button><a href="/article/10.3847/PSJ/ad9b24/meta" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="View article"><span class="icon-article"></span>View article<span class="offscreen-hidden">, Refined Mapping of Subsurface Water Ice on Mars to Support Future Missions</span></a><a href="/article/10.3847/PSJ/ad9b24/pdf" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="PDF"><span class="icon-file-pdf"></span>PDF<span class="offscreen-hidden">, Refined Mapping of Subsurface Water Ice on Mars to Support Future Missions</span></a><a href="/article/10.3847/PSJ/ad9b24/epub" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="ePub"><span class="icon-epub"></span><span class="offscreen-hidden">Download </span>ePub<span class="offscreen-hidden">, Refined Mapping of Subsurface Water Ice on Mars to Support Future Missions</span></a></div><div class="reveal-content"><div class="article-text view-text-small"><p>Mars has an extensive yet poorly understood cryosphere. Nevertheless, both direct and indirect evidence indicates extensive buried ice across the midlatitudes, including locations where it is presently unstable. While much progress has been made in exploring the processes responsible for ice deposition and preservation during recent climatic fluctuations, a global assessment of the multiple ice reservoirs remains elusive. Motivated by science and the need to find suitable human landing sites, the Mars Subsurface Water Ice Mapping (SWIM) project has developed techniques to map out buried ice. Through integration of all appropriate orbital data sets, the SWIM project produces ∼3 km pixel<sup>−1</sup> ice consistency maps over depth ranges of 0–1 m, 1–5 m, and >5 m. In concert with other studies, prior SWIM phases have recognized the uncertainty in our understanding of the geographic and vertical distribution of ice, especially between depths of 1 m and 10 m, creating a push for new ice-prospecting orbital missions, such as the International Mars Ice Mapper mission concept. Here we document the latest SWIM phase, which provides notional targeting maps of the lowest-latitude ice for future missions via a significant improvement in the geomorphic component of our work. The new mapping incorporates both an enhancement in our mapping of geomorphic features and surveys of thermal contraction crack polygons. Our results demonstrate the highly variable nature of the spatial distribution of the shallowest ground ice, with the most equatorward excursions occurring below 30° latitude N/S, locations thought to be out of equilibrium with the current climate.</p></div><div class="art-list-item-tools small wd-abstr-lower"><a class="mr-2" href="https://doi.org/10.3847/PSJ/ad9b24">https://doi.org/10.3847/PSJ/ad9b24</a></div></div></div></div><div class="art-list-item reveal-container reveal-closed"><div class="art-list-item-body"><div class="eyebrow"><span class="offscreen-hidden">The following article is </span><span class="red">Open access</span></div><a href="/article/10.3847/PSJ/ad644d" class="art-list-item-title event_main-link">On the Sensitivity of Apophis's 2029 Earth Approach to Small Asteroid Impacts</a><p class="small art-list-item-meta">Paul Wiegert 2024 <em>Planet. Sci. J.</em> <b>5</b> 184 </p><div class="art-list-item-tools small wd-abstr-upper"><button type="button" class="reveal-trigger mr-2 nowrap"><svg aria-hidden="true" class="fa-icon fa-icon--left fa-icon--flip" role="img" focusable="false" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 320 512"><path d="M137.4 374.6c12.5 12.5 32.8 12.5 45.3 0l128-128c9.2-9.2 11.9-22.9 6.9-34.9s-16.6-19.8-29.6-19.8L32 192c-12.9 0-24.6 7.8-29.6 19.8s-2.2 25.7 6.9 34.9l128 128z"/></svg><span class="reveal-trigger-label" data-reveal-text="Open abstract" data-reveal-label-alt="Close abstract" data-link-purpose-append="On the Sensitivity of Apophis’s 2029 Earth Approach to Small Asteroid Impacts" data-link-purpose-append-open="On the Sensitivity of Apophis’s 2029 Earth Approach to Small Asteroid Impacts">Open abstract</span></button><a href="/article/10.3847/PSJ/ad644d/meta" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="View article"><span class="icon-article"></span>View article<span class="offscreen-hidden">, On the Sensitivity of Apophis's 2029 Earth Approach to Small Asteroid Impacts</span></a><a href="/article/10.3847/PSJ/ad644d/pdf" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="PDF"><span class="icon-file-pdf"></span>PDF<span class="offscreen-hidden">, On the Sensitivity of Apophis's 2029 Earth Approach to Small Asteroid Impacts</span></a><a href="/article/10.3847/PSJ/ad644d/epub" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="ePub"><span class="icon-epub"></span><span class="offscreen-hidden">Download </span>ePub<span class="offscreen-hidden">, On the Sensitivity of Apophis's 2029 Earth Approach to Small Asteroid Impacts</span></a></div><div class="reveal-content"><div class="article-text view-text-small"><p>Apophis's current trajectory takes it safely past our planet at a distance of several Earth radii on 2029 April 13. Here the possibility is considered that Apophis could collide with a small asteroid, like the ones that frequently and unpredictably strike Earth, and the resulting perturbation of its trajectory. The probability of an impact that could significantly displace Apophis relative to its keyholes is found to be less than one in 10<sup>6</sup>, requiring a Δ<i>v</i> ≳ 0.3 mm s<sup>−1</sup>, while for an impact that could significantly displace Apophis compared to its miss distance in 2029, it is less than one in 10<sup>9</sup>, requiring a Δ<i>v</i> ≳ 5 cm s<sup>−1</sup>. These probabilities are below the usual thresholds considered by asteroid impact warning systems. Apophis is in the daytime sky and unobservable from mid-2021 to 2027. It will be challenging to determine from single-night observations in 2027 if Apophis has moved on the target plane enough to enter a dangerous keyhole, as the deviation from the nominal ephemeris might be only a few tenths of an arcsecond. An impending Earth impact would, however, be signaled clearly in most cases by deviations of tens of arcseconds of Apophis from its nominal ephemeris in 2027. Thus, most of the impact risk could be retired by a single observation of Apophis in 2027, though a minority of cases present some ambiguity and are discussed in more detail. Charts of the on-sky position of Apophis under different scenarios are presented for quick assessment by observers.</p></div><div class="art-list-item-tools small wd-abstr-lower"><a class="mr-2" href="https://doi.org/10.3847/PSJ/ad644d">https://doi.org/10.3847/PSJ/ad644d</a></div></div></div></div><div class="art-list-item reveal-container reveal-closed"><div class="art-list-item-body"><div class="eyebrow"><span class="offscreen-hidden">The following article is </span><span class="red">Open access</span></div><a href="/article/10.3847/PSJ/ad9a60" class="art-list-item-title event_main-link">JWST Near-infrared Spectroscopy of High-albedo Jupiter Trojans: A New Surface Type in the Trojan Belt</a><p class="small art-list-item-meta">Michael E. Brown <em>et al</em> 2025 <em>Planet. Sci. J.</em> <b>6</b> 22 </p><div class="art-list-item-tools small wd-abstr-upper"><button type="button" class="reveal-trigger mr-2 nowrap"><svg aria-hidden="true" class="fa-icon fa-icon--left fa-icon--flip" role="img" focusable="false" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 320 512"><path d="M137.4 374.6c12.5 12.5 32.8 12.5 45.3 0l128-128c9.2-9.2 11.9-22.9 6.9-34.9s-16.6-19.8-29.6-19.8L32 192c-12.9 0-24.6 7.8-29.6 19.8s-2.2 25.7 6.9 34.9l128 128z"/></svg><span class="reveal-trigger-label" data-reveal-text="Open abstract" data-reveal-label-alt="Close abstract" data-link-purpose-append="JWST Near-infrared Spectroscopy of High-albedo Jupiter Trojans: A New Surface Type in the Trojan Belt" data-link-purpose-append-open="JWST Near-infrared Spectroscopy of High-albedo Jupiter Trojans: A New Surface Type in the Trojan Belt">Open abstract</span></button><a href="/article/10.3847/PSJ/ad9a60/meta" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="View article"><span class="icon-article"></span>View article<span class="offscreen-hidden">, JWST Near-infrared Spectroscopy of High-albedo Jupiter Trojans: A New Surface Type in the Trojan Belt</span></a><a href="/article/10.3847/PSJ/ad9a60/pdf" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="PDF"><span class="icon-file-pdf"></span>PDF<span class="offscreen-hidden">, JWST Near-infrared Spectroscopy of High-albedo Jupiter Trojans: A New Surface Type in the Trojan Belt</span></a><a href="/article/10.3847/PSJ/ad9a60/epub" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="ePub"><span class="icon-epub"></span><span class="offscreen-hidden">Download </span>ePub<span class="offscreen-hidden">, JWST Near-infrared Spectroscopy of High-albedo Jupiter Trojans: A New Surface Type in the Trojan Belt</span></a></div><div class="reveal-content"><div class="article-text view-text-small"><p>We present 0.8–5 <i>μ</i>m JWST spectra of four ~20 km diameter Jupiter Trojans known to have albedos elevated above the values typical in the remaining Trojan population. The spectra of these four high-albedo Jupiter Trojans are all similar, with red slopes in the optical–IR transition region, a break to lower slopes at 1.3 <i>μ</i>m, and a broad absorptions from 2.8 to 4 <i>μ</i>m. The 0.8–2.5 <i>μ</i>m spectra of these objects match the spectra of neither the well-known "red" and "less-red" Jupiter Trojans nor of any known asteroid taxonomic class. The reflectivity of these objects does not rise redward of 4 <i>μ</i>m, a property that is seen in the previous JWST observations of Jupiter Trojans only in Polymele. Indeed, the high-albedo Jupiter Trojan spectra are a good match to that of Polymele, and Polymele is both the smallest Jupiter Trojan in the previous JWST sample and has the highest albedo of the objects in that sample. We conclude that Polymele and the other high-albedo Jupiter Trojans represent a third class of Jupiter Trojans not represented in the more heavily studied larger objects and are perhaps the products of recent disruptions. The Lucy flyby of Polymele in 2027 September will give a direct view of one of this new class of Jupiter Trojans.</p></div><div class="art-list-item-tools small wd-abstr-lower"><a class="mr-2" href="https://doi.org/10.3847/PSJ/ad9a60">https://doi.org/10.3847/PSJ/ad9a60</a></div></div></div></div></div></div></div></div><div tabindex="0" role="tabpanel" id="latest-articles-tab" aria-labelledby="latest-articles"><div class=" reveal-container reveal-closed reveal-enabled reveal-container--jnl-tab"><h2 class="tabpanel__title"><button type="button" class="reveal-trigger event_tabs-accordion" aria-expanded="false"><svg aria-hidden="true" class="fa-icon fa-icon--left fa-icon--flip" role="img" focusable="false" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 320 512"><path d="M137.4 374.6c12.5 12.5 32.8 12.5 45.3 0l128-128c9.2-9.2 11.9-22.9 6.9-34.9s-16.6-19.8-29.6-19.8L32 192c-12.9 0-24.6 7.8-29.6 19.8s-2.2 25.7 6.9 34.9l128 128z"/></svg>Latest articles</button></h2><div class="reveal-content tabpanel__content" style="display: none"><p><button data-reveal-label-alt="Close all abstracts" class="reveal-all-trigger mr-2 small" data-reveal-text="Open all abstracts" data-link-purpose-append="in this tab" data-link-purpose-append-open="in this tab"> Open all abstracts<span class="offscreen-hidden">, in this tab</span></button></p><div class="art-list"><div class="art-list-item reveal-container reveal-closed"><div class="art-list-item-body"><div class="eyebrow"><span class="offscreen-hidden">The following article is </span><span class="red">Open access</span></div><a href="/article/10.3847/PSJ/ada428" class="art-list-item-title event_main-link">Investigating Temporal and Spatial Variation of Jupiter's Atmosphere with Radio Observations</a><p class="small art-list-item-meta">Joanna Hardesty <em>et al</em> 2025 <em>Planet. Sci. J.</em> <b>6</b> 50 </p><div class="art-list-item-tools small wd-abstr-upper"><button type="button" class="reveal-trigger mr-2 nowrap"><svg aria-hidden="true" class="fa-icon fa-icon--left fa-icon--flip" role="img" focusable="false" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 320 512"><path d="M137.4 374.6c12.5 12.5 32.8 12.5 45.3 0l128-128c9.2-9.2 11.9-22.9 6.9-34.9s-16.6-19.8-29.6-19.8L32 192c-12.9 0-24.6 7.8-29.6 19.8s-2.2 25.7 6.9 34.9l128 128z"/></svg><span class="reveal-trigger-label" data-reveal-text="Open abstract" data-reveal-label-alt="Close abstract" data-link-purpose-append="Investigating Temporal and Spatial Variation of Jupiter’s Atmosphere with Radio Observations" data-link-purpose-append-open="Investigating Temporal and Spatial Variation of Jupiter’s Atmosphere with Radio Observations">Open abstract</span></button><a href="/article/10.3847/PSJ/ada428/meta" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="View article"><span class="icon-article"></span>View article<span class="offscreen-hidden">, Investigating Temporal and Spatial Variation of Jupiter's Atmosphere with Radio Observations</span></a><a href="/article/10.3847/PSJ/ada428/pdf" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="PDF"><span class="icon-file-pdf"></span>PDF<span class="offscreen-hidden">, Investigating Temporal and Spatial Variation of Jupiter's Atmosphere with Radio Observations</span></a><a href="/article/10.3847/PSJ/ada428/epub" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="ePub"><span class="icon-epub"></span><span class="offscreen-hidden">Download </span>ePub<span class="offscreen-hidden">, Investigating Temporal and Spatial Variation of Jupiter's Atmosphere with Radio Observations</span></a></div><div class="reveal-content"><div class="article-text view-text-small"><p>We study the spatial and temporal variability in Jupiter's atmosphere by comparing longitude-resolved brightness temperature maps from the Very Large Array radio observatory and NASA's Juno spacecraft Microwave Radiometer taken between 2013 and 2018. Spatial variations in brightness temperature, as observed at radio wavelengths, indicate dynamics in the atmosphere as they trace spatial fluctuations in radio-absorbing trace gases or physical temperature. We use four distinct frequency bands, probing the atmosphere from the water cloud region at the lowest frequency to the pressures above the ammonia cloud deck at the highest frequency. We visualize the brightness temperature anomalies and trace dynamics by analyzing the shapes of brightness temperature anomaly distributions as a function of frequency in Jupiter's North Equatorial Belt (NEB), Equatorial Zone (EZ), and South Equatorial Belt (SEB). The NEB has the greatest brightness temperature variability at all frequencies, indicating that more extreme processes are occurring there than in the SEB and EZ. In general, we find that the atmosphere at 5 and 22 GHz has the least variability of the frequencies considered, while observations at 10 and 15 GHz have the greatest variability. When comparing the size of the features corresponding to the anomalies, we find evidence for small-scale events primarily at the depths probed by the 10 and 15 GHz observations. In contrast, we find larger-scale structures deeper (5 GHz) and higher (22 GHz) in the atmosphere.</p></div><div class="art-list-item-tools small wd-abstr-lower"><a class="mr-2" href="https://doi.org/10.3847/PSJ/ada428">https://doi.org/10.3847/PSJ/ada428</a></div></div></div></div><div class="art-list-item reveal-container reveal-closed"><div class="art-list-item-body"><div class="eyebrow"><span class="offscreen-hidden">The following article is </span><span class="red">Open access</span></div><a href="/article/10.3847/PSJ/ada6aa" class="art-list-item-title event_main-link">Vertical and Temporal H<sub>3</sub><sup>+</sup> Structure at the Auroral Footprint of Io</a><p class="small art-list-item-meta">A. Mura <em>et al</em> 2025 <em>Planet. Sci. J.</em> <b>6</b> 49 </p><div class="art-list-item-tools small wd-abstr-upper"><button type="button" class="reveal-trigger mr-2 nowrap"><svg aria-hidden="true" class="fa-icon fa-icon--left fa-icon--flip" role="img" focusable="false" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 320 512"><path d="M137.4 374.6c12.5 12.5 32.8 12.5 45.3 0l128-128c9.2-9.2 11.9-22.9 6.9-34.9s-16.6-19.8-29.6-19.8L32 192c-12.9 0-24.6 7.8-29.6 19.8s-2.2 25.7 6.9 34.9l128 128z"/></svg><span class="reveal-trigger-label" data-reveal-text="Open abstract" data-reveal-label-alt="Close abstract" data-link-purpose-append="Vertical and Temporal H3+ Structure at the Auroral Footprint of Io" data-link-purpose-append-open="Vertical and Temporal H3+ Structure at the Auroral Footprint of Io">Open abstract</span></button><a href="/article/10.3847/PSJ/ada6aa/meta" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="View article"><span class="icon-article"></span>View article<span class="offscreen-hidden">, Vertical and Temporal H3+ Structure at the Auroral Footprint of Io</span></a><a href="/article/10.3847/PSJ/ada6aa/pdf" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="PDF"><span class="icon-file-pdf"></span>PDF<span class="offscreen-hidden">, Vertical and Temporal H3+ Structure at the Auroral Footprint of Io</span></a><a href="/article/10.3847/PSJ/ada6aa/epub" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="ePub"><span class="icon-epub"></span><span class="offscreen-hidden">Download </span>ePub<span class="offscreen-hidden">, Vertical and Temporal H3+ Structure at the Auroral Footprint of Io</span></a></div><div class="reveal-content"><div class="article-text view-text-small"><p>We report the first observation of the vertical and temporal structure of the H<sub>3</sub><sup>+</sup> emission at the auroral footprint of Io, as observed by Juno/JIRAM. The brightness vertical profile shows a maximum at 600 km above 1 bar, with no apparent difference between the main Alfvén wing (MAW) spot emission and the tail of the footprint. This observation better aligns with a broadband energy distribution of the precipitating electrons, instead of a monoenergetic one. The temporal profile of H<sub>3</sub><sup>+</sup> column density has been observed after the passage of the MAW and shows a hyperbolic decrease. A model of H<sub>3</sub><sup>+</sup> decay is proposed, which takes into account the second-order kinetics of dissociative recombination of H<sub>3</sub><sup>+</sup> ions with electrons. The model is found to be in very good agreement with Juno observations. The conversion factor from radiance to column density has been derived, as well as the half-life for H<sub>3</sub><sup>+</sup>, which is not constant but inversely proportional to the H<sub>3</sub><sup>+</sup> column density. This explains the wide range of H<sub>3</sub><sup>+</sup> lifetimes proposed before.</p></div><div class="art-list-item-tools small wd-abstr-lower"><a class="mr-2" href="https://doi.org/10.3847/PSJ/ada6aa">https://doi.org/10.3847/PSJ/ada6aa</a></div></div></div></div><div class="art-list-item reveal-container reveal-closed"><div class="art-list-item-body"><div class="eyebrow"><span class="offscreen-hidden">The following article is </span><span class="red">Open access</span></div><a href="/article/10.3847/PSJ/adabc1" class="art-list-item-title event_main-link">Stellar Occultation Observations of (38628) Huya and Its Satellite: A Detailed Look into the System</a><p class="small art-list-item-meta">F. L. Rommel <em>et al</em> 2025 <em>Planet. Sci. J.</em> <b>6</b> 48 </p><div class="art-list-item-tools small wd-abstr-upper"><button type="button" class="reveal-trigger mr-2 nowrap"><svg aria-hidden="true" class="fa-icon fa-icon--left fa-icon--flip" role="img" focusable="false" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 320 512"><path d="M137.4 374.6c12.5 12.5 32.8 12.5 45.3 0l128-128c9.2-9.2 11.9-22.9 6.9-34.9s-16.6-19.8-29.6-19.8L32 192c-12.9 0-24.6 7.8-29.6 19.8s-2.2 25.7 6.9 34.9l128 128z"/></svg><span class="reveal-trigger-label" data-reveal-text="Open abstract" data-reveal-label-alt="Close abstract" data-link-purpose-append="Stellar Occultation Observations of (38628) Huya and Its Satellite: A Detailed Look into the System" data-link-purpose-append-open="Stellar Occultation Observations of (38628) Huya and Its Satellite: A Detailed Look into the System">Open abstract</span></button><a href="/article/10.3847/PSJ/adabc1/meta" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="View article"><span class="icon-article"></span>View article<span class="offscreen-hidden">, Stellar Occultation Observations of (38628) Huya and Its Satellite: A Detailed Look into the System</span></a><a href="/article/10.3847/PSJ/adabc1/pdf" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="PDF"><span class="icon-file-pdf"></span>PDF<span class="offscreen-hidden">, Stellar Occultation Observations of (38628) Huya and Its Satellite: A Detailed Look into the System</span></a><a href="/article/10.3847/PSJ/adabc1/epub" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="ePub"><span class="icon-epub"></span><span class="offscreen-hidden">Download </span>ePub<span class="offscreen-hidden">, Stellar Occultation Observations of (38628) Huya and Its Satellite: A Detailed Look into the System</span></a></div><div class="reveal-content"><div class="article-text view-text-small"><p>The physical and orbital parameters of trans-Neptunian objects provide valuable information about the solar system's formation and evolution. In particular, the characterization of binaries provides insights into the formation mechanisms that may be playing a role at such large distances from the Sun. Studies show two distinct populations, and (38628) Huya occupies an intermediate position between the unequal-sized binaries and those with components of roughly equal sizes. In this work, we predicted and observed three stellar occultation events by Huya. Huya and its satellitewere detected during occultations in 2021 March and again in 2023 June. Additionally, an attempt to detect Huya in 2023 February resulted in an additional single-chord detection of the secondary. A spherical body with a minimum diameter of <i>D</i> = 165 km can explain the three single-chord observations and provide a lower limit for the satellite size. The astrometry of Huya's system, as derived from the occultations and supplemented by observations from the Hubble Space Telescope and Keck Observatory, provided constraints on the satellite orbit and the mass of the system. Therefore, assuming the secondary is in an equatorial orbit around the primary, the limb fitting was constrained by the satellite orbit position angle. The system density, calculated by summing the most precise measurement of Huya's volume to the spherical satellite average volume, is <i>ρ</i><sub>1</sub> = 1073 ± 66 kg m<sup>−3</sup>. The density that the object would have assuming a Maclaurin equilibrium shape with a rotational period of 6.725 ± 0.01 hr is <i>ρ</i><sub>2</sub> = 768 ± 42 kg m<sup>−3</sup>. This difference rules out the Maclaurin equilibrium assumption for the main body shape.</p></div><div class="art-list-item-tools small wd-abstr-lower"><a class="mr-2" href="https://doi.org/10.3847/PSJ/adabc1">https://doi.org/10.3847/PSJ/adabc1</a></div></div></div></div><div class="art-list-item reveal-container reveal-closed"><div class="art-list-item-body"><div class="eyebrow"><span class="offscreen-hidden">The following article is </span><span class="red">Open access</span></div><a href="/article/10.3847/PSJ/adaeb5" class="art-list-item-title event_main-link">How CO Affects the Composition of Titan's Tholins Generated with Electron Cyclotron Resonance Plasma</a><p class="small art-list-item-meta">Zhengbo Yang <em>et al</em> 2025 <em>Planet. Sci. J.</em> <b>6</b> 47 </p><div class="art-list-item-tools small wd-abstr-upper"><button type="button" class="reveal-trigger mr-2 nowrap"><svg aria-hidden="true" class="fa-icon fa-icon--left fa-icon--flip" role="img" focusable="false" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 320 512"><path d="M137.4 374.6c12.5 12.5 32.8 12.5 45.3 0l128-128c9.2-9.2 11.9-22.9 6.9-34.9s-16.6-19.8-29.6-19.8L32 192c-12.9 0-24.6 7.8-29.6 19.8s-2.2 25.7 6.9 34.9l128 128z"/></svg><span class="reveal-trigger-label" data-reveal-text="Open abstract" data-reveal-label-alt="Close abstract" data-link-purpose-append="How CO Affects the Composition of Titan’s Tholins Generated with Electron Cyclotron Resonance Plasma" data-link-purpose-append-open="How CO Affects the Composition of Titan’s Tholins Generated with Electron Cyclotron Resonance Plasma">Open abstract</span></button><a href="/article/10.3847/PSJ/adaeb5/meta" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="View article"><span class="icon-article"></span>View article<span class="offscreen-hidden">, How CO Affects the Composition of Titan's Tholins Generated with Electron Cyclotron Resonance Plasma</span></a><a href="/article/10.3847/PSJ/adaeb5/pdf" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="PDF"><span class="icon-file-pdf"></span>PDF<span class="offscreen-hidden">, How CO Affects the Composition of Titan's Tholins Generated with Electron Cyclotron Resonance Plasma</span></a><a href="/article/10.3847/PSJ/adaeb5/epub" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="ePub"><span class="icon-epub"></span><span class="offscreen-hidden">Download </span>ePub<span class="offscreen-hidden">, How CO Affects the Composition of Titan's Tholins Generated with Electron Cyclotron Resonance Plasma</span></a></div><div class="reveal-content"><div class="article-text view-text-small"><p>Titan's atmosphere possesses thick haze layers, but their formation mechanisms remain poorly understood, including the influence of oxygen-containing gas components on organic matter synthesis. As the most abundant oxygen-containing gas, the presence of <span xmlns:xlink="http://www.w3.org/1999/xlink" class="inline-eqn"><span class="tex"><span class="texImage"><img src="data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAAEAAAABCAQAAAC1HAwCAAAAC0lEQVR42mNkYAAAAAYAAjCB0C8AAAAASUVORK5CYII=" data-src="https://content.cld.iop.org/journals/2632-3338/6/2/47/revision1/psjadaeb5ieqn1.gif" style="max-width: 100%;" alt="${\rm{CO}}$" align="top"></img></span><script type="math/tex">{\rm{CO}}</script></span></span> has been found to exert a significant impact on the generation of oxygen-containing organic compounds. Therefore, investigating the influence of <span xmlns:xlink="http://www.w3.org/1999/xlink" class="inline-eqn"><span class="tex"><span class="texImage"><img src="data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAAEAAAABCAQAAAC1HAwCAAAAC0lEQVR42mNkYAAAAAYAAjCB0C8AAAAASUVORK5CYII=" data-src="https://content.cld.iop.org/journals/2632-3338/6/2/47/revision1/psjadaeb5ieqn2.gif" style="max-width: 100%;" alt="${\rm{CO}}$" align="top"></img></span><script type="math/tex">{\rm{CO}}</script></span></span> on the production and composition of tholins through laboratory simulations holds profound scientific significance in the context of Titan. The work presented here is an experimental simulation designed to evaluate the impact of <span xmlns:xlink="http://www.w3.org/1999/xlink" class="inline-eqn"><span class="tex"><span class="texImage"><img src="data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAAEAAAABCAQAAAC1HAwCAAAAC0lEQVR42mNkYAAAAAYAAjCB0C8AAAAASUVORK5CYII=" data-src="https://content.cld.iop.org/journals/2632-3338/6/2/47/revision1/psjadaeb5ieqn3.gif" style="max-width: 100%;" alt="${\rm{CO}}$" align="top"></img></span><script type="math/tex">{\rm{CO}}</script></span></span> on the atmospheric chemistry of Titan. To this end, <span xmlns:xlink="http://www.w3.org/1999/xlink" class="inline-eqn"><span class="tex"><span class="texImage"><img src="data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAAEAAAABCAQAAAC1HAwCAAAAC0lEQVR42mNkYAAAAAYAAjCB0C8AAAAASUVORK5CYII=" data-src="https://content.cld.iop.org/journals/2632-3338/6/2/47/revision1/psjadaeb5ieqn4.gif" style="max-width: 100%;" alt="${\rm{CO}}$" align="top"></img></span><script type="math/tex">{\rm{CO}}</script></span></span> was introduced into the standard <span xmlns:xlink="http://www.w3.org/1999/xlink" class="inline-eqn"><span class="tex"><span class="texImage"><img src="data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAAEAAAABCAQAAAC1HAwCAAAAC0lEQVR42mNkYAAAAAYAAjCB0C8AAAAASUVORK5CYII=" data-src="https://content.cld.iop.org/journals/2632-3338/6/2/47/revision1/psjadaeb5ieqn5.gif" style="max-width: 100%;" alt="${{\rm{N}}}_{2}/{\rm{C}}{{\rm{H}}}_{4}$" align="top"></img></span><script type="math/tex">{{\rm{N}}}_{2}/{\rm{C}}{{\rm{H}}}_{4}</script></span></span> mixture at varying mixing ratios from 0.2% to 9% and exposed to electron cyclotron resonance plasma to initiate photochemical reactions. Optical emission spectroscopy was employed for gas-phase in situ characterization, while infrared spectroscopy and high-resolution mass spectrometry were used to analyze the resulting solid products (tholins). Our results demonstrate that the addition of <span xmlns:xlink="http://www.w3.org/1999/xlink" class="inline-eqn"><span class="tex"><span class="texImage"><img src="data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAAEAAAABCAQAAAC1HAwCAAAAC0lEQVR42mNkYAAAAAYAAjCB0C8AAAAASUVORK5CYII=" data-src="https://content.cld.iop.org/journals/2632-3338/6/2/47/revision1/psjadaeb5ieqn6.gif" style="max-width: 100%;" alt="${\rm{CO}}$" align="top"></img></span><script type="math/tex">{\rm{CO}}</script></span></span> enriches the complexity of the chemical system. <span xmlns:xlink="http://www.w3.org/1999/xlink" class="inline-eqn"><span class="tex"><span class="texImage"><img src="data:image/png;base64,iVBORw0KGgoAAAANSUhEUgAAAAEAAAABCAQAAAC1HAwCAAAAC0lEQVR42mNkYAAAAAYAAjCB0C8AAAAASUVORK5CYII=" data-src="https://content.cld.iop.org/journals/2632-3338/6/2/47/revision1/psjadaeb5ieqn7.gif" style="max-width: 100%;" alt="${\rm{CO}}$" align="top"></img></span><script type="math/tex">{\rm{CO}}</script></span></span> not only supplies oxygen to the system but also enhances nitrogen's reactivity and incorporation, enhancing the number and quantity of the organic products.</p></div><div class="art-list-item-tools small wd-abstr-lower"><a class="mr-2" href="https://doi.org/10.3847/PSJ/adaeb5">https://doi.org/10.3847/PSJ/adaeb5</a></div></div></div></div><div class="art-list-item reveal-container reveal-closed"><div class="art-list-item-body"><div class="eyebrow"><span class="offscreen-hidden">The following article is </span><span class="red">Open access</span></div><a href="/article/10.3847/PSJ/adb02c" class="art-list-item-title event_main-link">Laboratory Study of Dust Mobilization on Airless Planetary Bodies in the Solar Wind Plasma</a><p class="small art-list-item-meta">A. Cabra <em>et al</em> 2025 <em>Planet. Sci. J.</em> <b>6</b> 46 </p><div class="art-list-item-tools small wd-abstr-upper"><button type="button" class="reveal-trigger mr-2 nowrap"><svg aria-hidden="true" class="fa-icon fa-icon--left fa-icon--flip" role="img" focusable="false" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 320 512"><path d="M137.4 374.6c12.5 12.5 32.8 12.5 45.3 0l128-128c9.2-9.2 11.9-22.9 6.9-34.9s-16.6-19.8-29.6-19.8L32 192c-12.9 0-24.6 7.8-29.6 19.8s-2.2 25.7 6.9 34.9l128 128z"/></svg><span class="reveal-trigger-label" data-reveal-text="Open abstract" data-reveal-label-alt="Close abstract" data-link-purpose-append="Laboratory Study of Dust Mobilization on Airless Planetary Bodies in the Solar Wind Plasma" data-link-purpose-append-open="Laboratory Study of Dust Mobilization on Airless Planetary Bodies in the Solar Wind Plasma">Open abstract</span></button><a href="/article/10.3847/PSJ/adb02c/meta" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="View article"><span class="icon-article"></span>View article<span class="offscreen-hidden">, Laboratory Study of Dust Mobilization on Airless Planetary Bodies in the Solar Wind Plasma</span></a><a href="/article/10.3847/PSJ/adb02c/pdf" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="PDF"><span class="icon-file-pdf"></span>PDF<span class="offscreen-hidden">, Laboratory Study of Dust Mobilization on Airless Planetary Bodies in the Solar Wind Plasma</span></a><a href="/article/10.3847/PSJ/adb02c/epub" class="mr-2 mb-0 nowrap event_mini-link" data-event-action="ePub"><span class="icon-epub"></span><span class="offscreen-hidden">Download </span>ePub<span class="offscreen-hidden">, Laboratory Study of Dust Mobilization on Airless Planetary Bodies in the Solar Wind Plasma</span></a></div><div class="reveal-content"><div class="article-text view-text-small"><p>Dust charging, and the subsequent mobilization and transport, have been suggested to explain a number of unresolved and unusual features observed on airless planetary surfaces. These processes are also critical for understanding and mitigating potential dust hazards to human and robotic exploration on the lunar surface. A patched charge model (PCM), developed from recent laboratory and theoretical studies, shows that secondary electrons and/or photoelectrons absorbed inside microcavities between dust particles on the surface of airless bodies can accumulate unexpectedly large negative charges, causing dust mobilization and lofting due to strong repulsive forces. Complementary to previous work with secondary electrons induced by an electron beam and/or photoelectrons induced by ultraviolet (UV) radiation, here we present dust mobilization due to ion-induced secondary electrons in a simulated solar wind plasma with the energies of nitrogen ions in the range of 100–1000 eV. It is shown that dust mobility is correlated with the secondary electron emission that is determined by the energy- and material-dependent emission yield, as well as the electrostatic potential profile developed above the surface. Our results provide a new charging mechanism by the solar wind plasma based on the PCM, which is expected to play an important role in dust mobilization in permanently shadowed regions, where the solar wind ions can be diverted onto areas that are not accessible to UV radiation.</p></div><div class="art-list-item-tools small wd-abstr-lower"><a class="mr-2" href="https://doi.org/10.3847/PSJ/adb02c">https://doi.org/10.3847/PSJ/adb02c</a></div></div></div></div></div></div></div></div></div></div></div></main><div class="db2 tb2"><div class="side-and-below"><div class="sidebar-list" id="wd-jnl-links"><h2 class="sidebar-list__heading">Journal links</h2><ul class="sidebar-list__list"><li><a href="https://aas.msubmit.net/cgi-bin/main.plex/"><b>Submit an article</b></a></li> <li><a href="https://iopscience.iop.org/journal/2632-3338/page/about-the-journal">About the journal</a></li> <li><a href="https://journals.aas.org/manuscript-preparation/">Author instructions</a></li> <li><a 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