Icarus最新文献

{"title":"Landslide chronology on mars: A window into the past of Valles Marineris and martian slopes","authors":"Giovanni Battista Crosta,&nbsp;Fabio Vittorio De Blasio,&nbsp;Elena Valbuzzi,&nbsp;Alessandro Martinazzi","doi":"10.1016/j.icarus.2025.116653","DOIUrl":"10.1016/j.icarus.2025.116653","url":null,"abstract":"<div><div>Martian landslide deposits provide valuable insights into the planet's geomorphological evolution. Their degree of preservation is such that they can be recognized after billions of years. Therefore, a study of Martian landslides may reveal clues as to the surface and environmental conditions at the moment of collapse. In particular, determining their age is of great importance for reconstructing the geomorphological and structural evolution of the Martian surface. We conducted a comprehensive age dating analysis of 32 clusters, encompassing 102 landslides and 38 non-landslide units across various Martian regions. Most of the landslides dated in this work are considered here for the first time, while for several others we present an updating of their age, allowing for a validation of previous dating, and a broader geomorphological interpretation. Important factors affecting age determination such as landslide type, secondary craters, and resurfacing processes have been examined in detail to improve data quality and provide more robust conclusions. While very low frequency of slope collapse is observed between 3.2 and 2.4 Ga after a period of higher instability as confirmed by fluvial and glacial features, the overall trend of increasing frequency with time remains dominant. This is consistent with previous studies, and is now supported by a significantly larger dataset which modifies existing age determinations. This suggests the presence of a large number of ancient undetected landslides, buried beneath more recent deposits. This research provides new insights into the timing and frequency of mass wasting events on Mars, contributing to a better understanding of the planet's geomorphological evolution.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"439 ","pages":"Article 116653"},"PeriodicalIF":2.5,"publicationDate":"2025-05-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144139384","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Measurement of viscous erosion rate from plume surface interactions in low-pressure environments","authors":"B. Dotson,&nbsp;D. Britt,&nbsp;P. Metzger","doi":"10.1016/j.icarus.2025.116654","DOIUrl":"10.1016/j.icarus.2025.116654","url":null,"abstract":"<div><div>Experimental measurements of viscous erosion rate with regolith simulants were completed under vacuum conditions with a splitter plate, plume cratering setup and non-reacting flows. Using Lunar Highlands Simulant (LHS-1), Lunar Mare Simulant (LMS-1), LHS-1D (Dust) Simulants, this study examined the impacts of bulk density and mass flow rate on crater morphology and viscous erosion rate with ambient pressures between 2 and 760,000 mTorr. Results show that crater shape changes as a function of ambient pressure, owing to plume expansion under vacuum conditions, resulting in annular craters below 1000 mTorr. Erosion rate and ejecta streaking appears to be dependent on the Knudsen number (<em>Kn</em>) and increases with a decrease in ambient pressure. When compared to the continuum region (<em>Kn</em> ≤ 0.1), viscous erosion rate is higher in the free-molecular region (<em>Kn</em> ≥ 10), but the highest measured erosion rates were noted in the transition region (0.1 &lt; <em>Kn</em> &lt; 1) which best corresponds to Martian ambient conditions. A modified version of <span><span>Metzger's (2024a)</span></span> equation for volumetric erosion rate is presented using empirical fits for lunar mare and highlands regolith simulants, with limitations discussed. Measurements show that mass flow rate and bulk density can influence viscous erosion rate by 30 % under vacuum conditions, particularly in the free-molecular region. While cohesion clearly influences erosion rate, results suggest that plume dynamics, porosity, and surface roughness may also play an important role in rarified conditions such as on the Moon. To help protect personnel and equipment on future missions, models of plume surface interactions should incorporate these modified equations for viscous erosion.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"439 ","pages":"Article 116654"},"PeriodicalIF":2.5,"publicationDate":"2025-05-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144099387","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Putative biosignatures in hydrovolcanic tuffs from a Mars-relevant environment: Western Snake River Plain volcanic field, Idaho","authors":"Catheryn H. Ryan ,&nbsp;Mariek E. Schmidt ,&nbsp;Gordon R. Osinski","doi":"10.1016/j.icarus.2025.116642","DOIUrl":"10.1016/j.icarus.2025.116642","url":null,"abstract":"<div><div>Hydrovolcanic tuffs formed through magma-water interactions in lacustrine or littoral environments have been found to contain micro-textural elements, including microtubules and granular textures, within glass fragments. The morphological and associated geochemical characteristics of these micro-textures show evidence that they are formed by microbially-mediated dissolution of basaltic glass in an aqueous setting, establishing them as likely biosignatures. Further, the terrestrial setting of these samples and their basaltic composition is analogous to environmental conditions expected to have existed throughout the history of Mars.</div><div>We present the first report of putative biogenic alteration textures in basaltic glass from the Pliocene-Pleistocene hydrovolcanoes of the Western Snake River Plain volcanic field, Idaho, USA. Samples collected from tuff cones, tuff rings, and maars which erupted into paleo-Lake Idaho contain microtubules and granular alteration comparable in morphology (diameter, length, curvature, internal contents, branching) and size distribution to those recorded in other terrestrial hydrovolcanic fields. Petrographic relationships between fresh glass containing microtubules, glass that has been fully altered to palagonite, and mineral-filled vesicles and fractures indicate that tubules formed under low-temperature aqueous alteration conditions during the palagonitization process and ongoing alteration mineral precipitation. Alteration minerals including calcite and zeolites show that these fluids likely did not exceed 80 °C in temperature. Major element mapping of vitric clasts in hydrovolcanic tuff revealed most elements are depleted or neutral within microtubule interiors relative to the surrounding glass, although iron and titanium were notably enriched in many tubules. We found little distinction in major element composition between microtexture-bearing and non-microtexture-bearing glasses, with the exception of some microtexture-bearing samples being depleted in Na₂O compared to the non-microtexture-bearing glass. Western Snake River Plain is relevant to Mars in terms of geochemical, mineralogical, and environmental context; and this setting is capable of preserving putative biosignatures. This work has implications for furthering our understanding of how these microtextures are formed and preserved, and for potential astrobiological investigation of Mars.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"439 ","pages":"Article 116642"},"PeriodicalIF":2.5,"publicationDate":"2025-05-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144099388","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Tholin formation and accumulation due to hypersonic high-temperature flows in methane-containing atmospheres","authors":"Marcello Lappa ,&nbsp;Antonio Esposito ,&nbsp;Carmela Russo ,&nbsp;Barbara Apicella","doi":"10.1016/j.icarus.2025.116649","DOIUrl":"10.1016/j.icarus.2025.116649","url":null,"abstract":"<div><div>We report on another tholins formation mechanism relying on the high energies typically available in hypersonic flows. The considered conditions are representative of vehicle or meteorite entry in atmospheres containing the required precursor molecules. It is shown that the involved high temperatures can break the chemical bonds in methane molecules, thereby releasing carbon atoms in the gas mixture. These can combine with the other species and form various compounds with a variable degree of carbon depending on the local conditions in which the reaction takes place. Notably, the variability in composition also depends on the specific path followed by molecules in the gas flow. The presence of sudden expansions or localized shock waves in the current and the ensuing variations in pressure and temperature, have a non-negligible effect on the nature of the organic residues. These have been characterized by an array of chemical and spectroscopic techniques: atmospheric pressure photoionization mass spectrometry (APPI-MS), elemental analysis, infrared absorption (FT-IR), UV–visible absorption and fluorescence. Moreover, some effort was provided to correlate them with the thermochemical and fluid-dynamic conditions occurring in the hypersonic wind tunnel used for the experiments. Overall, such results suggest a novel possible route to the formation of tholins, which is still poorly known and hitherto scarcely investigated.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"439 ","pages":"Article 116649"},"PeriodicalIF":2.5,"publicationDate":"2025-05-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144083873","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The bright-field grinding tomography of coarse-grained calcium‑aluminum-rich inclusions in the Allende meteorite","authors":"Ryota Fukai ,&nbsp;Yusuke Takeda ,&nbsp;Yuki Masuda ,&nbsp;Daiki Yamamoto ,&nbsp;Yasuhiro Iba ,&nbsp;Shintaro Sasaki ,&nbsp;Shin Ikegami ,&nbsp;Aya Kubota ,&nbsp;Reo Sato ,&nbsp;Tomohiro Usui","doi":"10.1016/j.icarus.2025.116648","DOIUrl":"10.1016/j.icarus.2025.116648","url":null,"abstract":"<div><div>The evolution associated with coagulation/fragmentation processes of dust to planetesimals in the protosolar disk is the critical phase of planet formation in the Solar System. The meteoritic components, such as calcium‑aluminum-rich inclusions (CAIs), will provide essential constraints on the coagulation/fragmentation process in the early stage of the disk. We applied the bright-field grinding tomography method to an Allende meteorite (CV3) slab to visualize the coarse-grained CAIs (CG-CAIs) in a colorized 3D model with high spatial resolution. We found four mm-scale CG-CAIs that experienced deformation and/or fragmentation processes within ∼1.8 × 10³ mm³ Allende slab. An angular-shaped CG-CAI's surface showed the anisotropy of red-gray and white sides, which suggests that the fragmentation results in the loss of the primitive Wark-Lovering rim. We also found a vesicular-shaped CG-CAI, which indicates that the fracturing and complex formation process of this CG-CAI likely proceeded prior to the accretion of the Wark-Lovering rim. Our observations reveal that the fragmentation of Allende CAIs occurred during the parent body accretion stage and also in the protosolar disk.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"439 ","pages":"Article 116648"},"PeriodicalIF":2.5,"publicationDate":"2025-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144099318","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Spectral hydration features in nominally anhydrous minerals & implications for lunar remote sensing","authors":"Kierra A. Wilk ,&nbsp;J.L. Bishop ,&nbsp;A. Maturilli ,&nbsp;C.M. Pieters ,&nbsp;J.F. Mustard ,&nbsp;K. Robertson","doi":"10.1016/j.icarus.2025.116651","DOIUrl":"10.1016/j.icarus.2025.116651","url":null,"abstract":"<div><div>The contributions of external and internal hydration (OH and H₂O) on the shape and strength of hydration related features at 3 and 6 μm for lunar relevant nominally anhydrous minerals were investigated under vacuum conditions. Understanding the effect of hydration on the reflectance spectra of lunar analog materials in the laboratory can provide insights into remote sensing observations of the lunar surface and the potential for 3 and/or 6 μm observations to determine the speciation of hydration on the Moon. We demonstrate changes in the shape and strength of the broad 3 μm absorption feature in olivine and anorthite that is associated with the removal of hydration under changing environmental conditions. The overlapping nature of OH and H₂O related absorption features in the ∼3 μm region makes it difficult to uniquely determine the speciation of hydration. Despite evidence of H₂O loss in the 3 μm region, we do not observe the fundamental bending mode of H₂O at 6 μm, posing potential challenges for the detection H₂O on the lunar surface and throughout our solar system.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"438 ","pages":"Article 116651"},"PeriodicalIF":2.5,"publicationDate":"2025-05-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144069237","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Volcanism along the rings of the Crisium Basin on the Moon: Insights from M3 onboard Chandrayaan - 1","authors":"Neha Panwar ,&nbsp;Neeraj Srivastava ,&nbsp;Ankita Yadav ,&nbsp;Megha Bhatt ,&nbsp;Christian Wöhler ,&nbsp;Anil Bhardwaj","doi":"10.1016/j.icarus.2025.116641","DOIUrl":"10.1016/j.icarus.2025.116641","url":null,"abstract":"<div><div>The Crisium Basin (17.0°N, 59.1°E) is a Nectarian multi-ring basin hosting extensive volcanism inside the basin center and along its four rings. The Crisium Basin is an essential proxy for understanding basin-related magmatic activity on the Moon. A detailed stratigraphy and chronology have been established for the Mare Crisium in several earlier studies. However, there has been no comprehensive study regarding the composition and emplacement timescales of the basalts along the rings of the Crisium Basin. The basalts along the rings of the Crisium Basin have been emplaced within Mare Undarum, Mare Spumans, Mare Anguis, Cleomedes Crater, and Lacus Bonitatis. Our recent study identified Marginis West as an episode of volcanism along the outermost ring of the Crisium Basin. This study, for the first time, examines the compositional diversity and ages of the basalts emplaced along the rings of the Crisium Basin to better understand its geological evolution. We report the youngest volcanic unit emplaced inside the Crisium Basin at ∼2.0 Ga inside Mare Anguis. Based on the spectral signatures, we report that the contemporaneously formed mare units within the Crisium Basin are compositionally different, displaying a westward increase in Ca, and large pre-existing crustal structures would have deeply influenced the volcanism within the basin in the region.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"438 ","pages":"Article 116641"},"PeriodicalIF":2.5,"publicationDate":"2025-05-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144069238","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Estimates of rotation periods for Jupiter Trojans with the Zwicky Transient Facility photometric lightcurves","authors":"Zhuofu (Chester) Li ,&nbsp;Yasin A. Chowdhury ,&nbsp;Željko Ivezić ,&nbsp;Ashish Mahabal ,&nbsp;Ari Heinze ,&nbsp;Lynne Jones ,&nbsp;Mercedes S. Thompson ,&nbsp;Eric Bellm ,&nbsp;Mario Jurić ,&nbsp;Andrew J. Connolly ,&nbsp;Bryce Bolin ,&nbsp;Frank J. Masci ,&nbsp;Avery Wold ,&nbsp;Reed L. Riddle ,&nbsp;Richard G. Dekany","doi":"10.1016/j.icarus.2025.116609","DOIUrl":"10.1016/j.icarus.2025.116609","url":null,"abstract":"<div><div>We present new rotational period estimates for 216 Jupiter Trojans using photometric data from the Zwicky Transient Facility (ZTF), including 80 Trojans with previously unknown periods. Our analysis reveals rotation periods ranging from 4.6 h to 447.8 h. These results support the existence of a spin barrier for Trojans larger than 10 km, with periods clustering between 4 and 4.8 h. This spin barrier is roughly twice as long as that observed for main-belt asteroids, suggesting that Jupiter Trojans have significantly lower bulk densities, likely due to a higher fraction of ices and volatile materials in their composition. We identify three new Trojans with reliable rotation periods near the spin barrier, doubling the number of known Trojans in this critical period range. Using these results, we estimate a mean density of <span><math><mrow><mo>∼</mo><mn>0</mn><mo>.</mo><mn>52</mn><mspace></mspace><msup><mrow><mi>g/cm</mi></mrow><mrow><mn>3</mn></mrow></msup></mrow></math></span> for rubble-pile Trojans. Our findings contribute to the growing body of evidence that many Trojans are rubble-pile bodies with distinct physical properties compared to main-belt asteroids. Looking forward, we anticipate that forthcoming data from the Vera C. Rubin Observatory’s Legacy Survey of Space and Time (LSST) will provide rotational period estimates for several hundred thousand Trojans, down to objects as small as 1 km, enabling a more detailed investigation of their rotational properties and internal structure.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"438 ","pages":"Article 116609"},"PeriodicalIF":2.5,"publicationDate":"2025-05-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143942603","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Planetary surface dating from crater size–frequency distribution measurements: Sequence probability and simultaneous formation. Did the close Chang'E-6 mare units form simultaneously?","authors":"Greg Michael,&nbsp;Li Zhang,&nbsp;Congzhe Wu,&nbsp;Jianzhong Liu","doi":"10.1016/j.icarus.2025.116644","DOIUrl":"10.1016/j.icarus.2025.116644","url":null,"abstract":"<div><div>The Chang'e-6 lunar spacecraft returned samples from the southern mare of the Apollo basin. This work analyses the likelihood that a set of six close crater dating measurements of sub-units near the sampling site actually represent a single formation event. Using theoretical considerations, we find that the measurements are consistent with a simultaneous formation hypothesis with about 1 in 6 likelihood, so that a close sequential formation is more probable. Results of radioisotope dating of basaltic fragments from the surface scoop sample were recently reported close to 2.8 Ga. Our crater dating of the vicinity suggests that the upper 2–17 m predominantly records an age of <span><math><mi>μ</mi><msubsup><mn>1.66</mn><mrow><mo>−</mo><mn>0.054</mn></mrow><mrow><mo>+</mo><mn>0.053</mn></mrow></msubsup><mspace></mspace><mi>Ga</mi></math></span>, which points to the samples' formation predating this crater population reset of the surface.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"438 ","pages":"Article 116644"},"PeriodicalIF":2.5,"publicationDate":"2025-05-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143947441","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Impact-induced fayalite glass from Chang'e-5 regolith revealed by electron pair distribution function and ReaxFF molecular dynamics","authors":"Hongmei Yang ,&nbsp;Haiyang Xian ,&nbsp;Jianxi Zhu ,&nbsp;Xiao Wu ,&nbsp;Shan Li ,&nbsp;Xiaoju Lin ,&nbsp;Jiaxin Xi ,&nbsp;Yiping Yang ,&nbsp;Hongping He","doi":"10.1016/j.icarus.2025.116643","DOIUrl":"10.1016/j.icarus.2025.116643","url":null,"abstract":"<div><div>Impacts play a vital role in lunar formation and evolution. The mineral phase transformations induced by impacts are crucial for understanding the impact processes, such as the amorphization of olivine. In this study, we investigated the formation mechanism of fayalite glass in Chang'e-5 breccia using the electron pair distribution function and molecular dynamics simulations. The results show that fayalite glass formed during pressure release, with temperatures ranging from 3200 to 3400 K before fayalite melt quenching and a residual pressure of around 1 GPa. By integrating micro-regional analyses, the results suggest that impact-induced particle fragmentation creates shear surfaces, where particle friction generates enough heat to cause local melting of fayalite, followed by rapid quenching to produce the glass. This study provides a microscopic perspective on the formation mechanism of impact glass, enhancing our understanding of the impact processes in the solar system.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"438 ","pages":"Article 116643"},"PeriodicalIF":2.5,"publicationDate":"2025-05-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143947442","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}