Icarus最新文献

{"title":"Iron isotopes of Chang'e-5 soil and mineral components: Implications for post-eruption processes on lunar surface","authors":"Yiheng Li ,&nbsp;Zaicong Wang ,&nbsp;Yuqi Qian ,&nbsp;Wen Zhang ,&nbsp;Yantong Feng ,&nbsp;Hong Liu ,&nbsp;Keqing Zong ,&nbsp;Qi He ,&nbsp;Zhenbing She ,&nbsp;Xiang Wu ,&nbsp;Ming Li ,&nbsp;Zhaochu Hu ,&nbsp;Long Xiao ,&nbsp;Yang Li ,&nbsp;Frederic Moynier","doi":"10.1016/j.icarus.2024.116362","DOIUrl":"10.1016/j.icarus.2024.116362","url":null,"abstract":"<div><div>Due to rapid magma cooling and extensive space weathering, significant disequilibrium crystallization and secondary modification widely occur in lunar mare basalt after its eruption on the lunar surface. In this study, we conducted bulk and in-situ Fe isotope analyses to investigate the post-eruption processes on Chang'e-5 (CE-5) samples. The CE-5 soil shows a minor elevation of δ⁵⁶Fe value (∼0.05 ‰) relative to the CE-5 basalt clasts. Correlations between Ni and Cu contents with δ⁵⁶Fe values suggest that the minor increase in the δ⁵⁶Fe from the CE-5 basalt to soil primarily occurred during evaporation caused by meteorite impacts. Such isotopic variation between CE-5 basalt and soils is notably lower than what is observed for Apollo samples and reflects the low maturity of CE-5 soils. This is consistent with the low Is/FeO value constrained by magnetic approaches. Therefore, measuring the δ⁵⁶Fe values of lunar soil is suitable to evaluate the degrees of maturity for lunar soils due to space weathering. In-situ analyses of δ⁵⁶Fe reveal significant variations in different grains of olivine (δ⁵⁶Fe: −0.57 to −0.17 ‰) and ilmenite (−0.06 to +0.42 ‰) and also in their interior (mainly for olivine). These δ⁵⁶Fe variations in minerals can be ascribed to the disequilibrium crystallization of lava flow and fast cooling, which is consistent with conclusions based on petrologic observations such as its extensive differentiation and silicate liquid immiscibility. Therefore, the post-eruption processes on the lunar surface could lead to significant variations in isotopic compositions at different scales of basalts, which in turn record the history of late-stage magma evolution and space weathering on the lunar surface.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"426 ","pages":"Article 116362"},"PeriodicalIF":2.5,"publicationDate":"2024-10-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142578749","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":"Three-dimensional modeling of Ganymede’s Chapman–Ferraro magnetic field and its role in subsurface ocean induction","authors":"Nawapat Kaweeyanun ,&nbsp;Adam Masters","doi":"10.1016/j.icarus.2024.116356","DOIUrl":"10.1016/j.icarus.2024.116356","url":null,"abstract":"<div><div>In April 2023, the Jupiter Icy Moons Explorer (Juice) began its journey to orbit Jupiter’s largest and only magnetic moon, Ganymede. Part of the mission’s objectives aim to verify existence of the moon’s subsurface ocean and determine its structure through its induced response to external excitation by periodically varying magnetic field. Known contributions to the excitation are those from Jupiter’s dipole (at synodic period) and quadrupole (at half-synodic period) variations, and Ganymede’s inclined eccentric orbit around Jupiter (at orbital period). We propose that Ganymede’s magnetopause, where the Chapman–Ferraro (C–F) magnetic field arises from local currents, also contributes to subsurface ocean induction. This article introduces the first three-dimensional model of the C–F field and its outputs at Ganymede’s subsurface ocean and larger magnetosphere. The field is shown to be non-uniform — strongest near upstream Ganymede’s subflow region and gradually weakening away from it. Magnetopause asymmetry due to the Jovian guide field results in largely synodic variation of the C–F field, with exceptions near Ganymede’s equator and subflow meridian where asymmetry effects are minimal and the variations are half-synodic. The C–F field amplitude is of general order <span><math><mrow><mo>∼</mo><mn>50</mn></mrow></math></span> nT, which is significant relative to excitation from the Jovian field. Comparisons to Galileo data and magnetohydrodynamic simulation results suggest the model is useful, therefore the magnetopause effects must be considered in future induction modeling of Ganymede’s subsurface ocean ahead of the Juice mission.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"426 ","pages":"Article 116356"},"PeriodicalIF":2.5,"publicationDate":"2024-10-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142572881","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Seasonal and interannual variability of the water vapor vertical distribution in the Martian lower atmosphere","authors":"Alexey A. Pankine ,&nbsp;Timothy H. McConnochie ,&nbsp;Michael D. Smith","doi":"10.1016/j.icarus.2024.116360","DOIUrl":"10.1016/j.icarus.2024.116360","url":null,"abstract":"<div><div>We apply a novel method to retrieve water vapor vertical distributions in the Martian atmosphere to spectra collected by the Mars Global Surveyor (MGS) Thermal Emission Spectrometer (TES). The new method exploits differences in sensitivity of the daytime and nighttime TES nadir spectra to water vapor content in different parts of the lower atmosphere (0–40 km). Based on the test retrievals from simulated environments, vertical profiles of water vapor can be retrieved with accuracy ∼20–40 % depending on the season and altitude above surface. Retrievals from observations collected by the MGS TES between L_s = 135° in MY24 and L_s = 75° in MY27 enable exploration of the seasonal and interannual variabilities of the vertical distribution of water vapor. Retrieved vapor distributions and their seasonal variability are generally consistent with those predicted by a numerical circulation model. Vapor is concentrated near the surface in the northern polar region and the mid-latitudes during the northern summer (L_s = 90°). During the southern summer (L_s = 270°) vapor extends higher in the atmosphere in the southern polar region, reflecting both sublimation of the seasonal surface ice and atmospheric transport by the upper branch of the southern Hadley cell. During both equinoxes (L_s = 0° and L_s = 180°) vapor is found in the lower part of the tropical atmosphere. At the same time the retrieved vertical distributions exhibit notable interannual variability. Following the global dust storm of MY25, vapor is confined to lower altitudes in the southern polar region during the southern summer. During the southern spring in MY26 (L_s = 180°-270°) vapor extends higher in the atmosphere and mixing ratios increase faster with height at the equator and in the northern tropics. These examples suggest that Martian atmosphere may experience interannual changes in the atmospheric transport, some of which could be in response to global dust storm events.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"426 ","pages":"Article 116360"},"PeriodicalIF":2.5,"publicationDate":"2024-10-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142578747","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":"Changes in the longitude polarization dependence of Jupiter's moon Io as evidence of the long-term variability of its volcanic activity","authors":"Nikolai N. Kiselev ,&nbsp;Herman G. Dyachenko ,&nbsp;Nikolai V. Karpov ,&nbsp;Kirill A. Antoniuk","doi":"10.1016/j.icarus.2024.116351","DOIUrl":"10.1016/j.icarus.2024.116351","url":null,"abstract":"<div><div><strong>The aim of the work was to investigate the longitude (orbital) dependence of the polarization of Jupiter's moon Io and compare results of our study with what is reported in the literature.</strong> We used our published observations and supplemented them with new measurements carried out with the polarimeters mounted on the 2.6 m Shajn telescope of the Crimean Astrophysical Observatory and the 2 m telescope of the Peak Terskol Observatory in the UBVRI bands at phase angles between 10° and 12° in August 2023 – February 2024. We have determined that amplitude of the orbital polarization in the V band does not exceed ≈0.1 %. It is the deepest −0.17 ± 0.03 % at L ≈ 270° and the shallowest −0.07 ± 0.03 % near L ≈ 130°. These parameters differ markedly from that obtained by <span><span>Zellner and Gradie (1975)</span></span>, which found that the orbital polarization variations from 0.4 to 0.5 % for α &gt; 10°, and the negative branch is the deepest near L = 160° and the shallowest near L = 300°. These differences may be a consequence of changes in the reflective properties of the local areas of Io's surface due to long-term changes in Io's local or global volcanic activity.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"426 ","pages":"Article 116351"},"PeriodicalIF":2.5,"publicationDate":"2024-10-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142560985","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":"New astrometric positions for six Jovian irregular satellites using Gaia DR3 in 2016 — 2021","authors":"X. Lu ,&nbsp;Q.Y. Peng ,&nbsp;A. Vienne ,&nbsp;X.Q. Fang ,&nbsp;F.R. Lin","doi":"10.1016/j.icarus.2024.116352","DOIUrl":"10.1016/j.icarus.2024.116352","url":null,"abstract":"<div><div>The Jovian system is like a miniature solar system, with the system being more than twice as massive as all the other planets combined and having many natural satellites. Its formation and early evolution had a profound influence on our knowledge of the sculpting of the architecture of the solar system. Astrometric observations are of importance, based on these observations, its orbital dynamics, as well as its origin sometimes, of a solar system object can be determined. We aimed to obtain good astrometric positions of some irregular satellites Elara, Pasiphae, Sinope, Lysithea, Carme and Ananke to refine their orbits and ephemerides, and to understand their dynamics. We have taken, processed and reduced 964 ground-based CCD frames obtained between 2016 and 2021 by the 2.4 m telescope at the Lijiang Station of Yunnan Observatory over 27 nights. Among CCD image processing, the image subtraction technique of ISIS is employed to eliminate star images that are close to or/and almost overlapped with those of our targets in 2019. The star catalog Gaia DR3 is utilized for astrometric calibration, in which a weight scheme is applied to solve more accurate plate model. For all targets, their theoretical positions are retrieved from the Institut de Mécanique Céleste et de Calcul des Éphémérides (IMCCE) ephemeris. Our results show the mean (O - C)s (observed minus computed) of the positional residuals of all targets are <span><math><mrow><mo>−</mo><msup><mrow><mn>0</mn></mrow><mrow><mo>′</mo><mo>′</mo></mrow></msup><mo>.</mo><mn>007</mn></mrow></math></span> and <span><math><mrow><msup><mrow><mn>0</mn></mrow><mrow><mo>′</mo><mo>′</mo></mrow></msup><mo>.</mo><mn>011</mn></mrow></math></span> in R.A. and Dec., respectively. Their corresponding standard deviations are about <span><math><mrow><msup><mrow><mn>0</mn></mrow><mrow><mo>′</mo><mo>′</mo></mrow></msup><mo>.</mo><mn>05</mn></mrow></math></span> in each direction, except for Ananke (the faintest satellite) with its standard deviation about <span><math><mrow><msup><mrow><mn>0</mn></mrow><mrow><mo>′</mo><mo>′</mo></mrow></msup><mo>.</mo><mn>08</mn></mrow></math></span> in each direction.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"426 ","pages":"Article 116352"},"PeriodicalIF":2.5,"publicationDate":"2024-10-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142552390","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":"NAROO program: Analysis of USNO Galilean observations 1967–1998","authors":"V. Robert ,&nbsp;D. Pascu ,&nbsp;V. Lainey ,&nbsp;J.-E. Arlot","doi":"10.1016/j.icarus.2024.116344","DOIUrl":"10.1016/j.icarus.2024.116344","url":null,"abstract":"<div><div>The New Astrometric Reduction of Old Observations (NAROO) program is dedicated to the measurement of astrophotographic plates and the analysis of old observations for scientific purposes. One of the main objectives of the NAROO program is to provide accurate positional measurements of planets and satellites to improve our knowledge of their orbits and dynamics, and to infer the accuracy of the planet and satellite ephemerides. We digitized 553 astronegatives of the Galilean satellites taken with the McCormick 26-inch refractor in 1967/68 and the U.S. Naval Observatory 26-inch refractor from 1973 to 1998, resulting in 2650 individual observations. We measured and reduced these observations through an optimal process that includes image, instrumental, and spherical corrections using Gaia-DR3 catalog to provide the most accurate equatorial (RA, Dec) ICRS (Gaia-CRF3) positions. 4819 positions of the Galilean satellites have been determined with an accuracy of 55 mas (160 km at Jupiter), near the limit of the photographic technique for such work. These data can help to improve the equatorial positions of Jupiter. They also can be used in the context of quantifying tidal effects and will still be useful when Europa Clipper and Juice data will become available.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"426 ","pages":"Article 116344"},"PeriodicalIF":2.5,"publicationDate":"2024-10-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142572947","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Expected constraints on Phobos interior from the MMX gravity and rotation observations","authors":"Alfonso Caldiero,&nbsp;Sébastien Le Maistre","doi":"10.1016/j.icarus.2024.116343","DOIUrl":"10.1016/j.icarus.2024.116343","url":null,"abstract":"<div><div>The origin of the Martian moons is still uncertain, and knowledge about their interior could provide support to some of its leading theories. In preparation for the JAXA Martian Moons eXploration (MMX) mission, we review our current knowledge on the interior of Phobos, and provide synthetic tests showing how the gravity and rotation determination could allow the detection of specific interior-structure properties. The inversion of the geodetic observables for the retrieval of the internal mass distribution of a set of synthetic interior models is performed via non-linear least-squares, where the interior parameterization is based on the level-set method. We additionally provide simple expressions allowing to relate some of these interior models to the geodetic observables of Phobos. The results, based on realistic measurement resolution and noise scenarios, show good retrievals for most of the models at the data resolutions expected from MMX. Specifically, we find the gravity information is realistically sufficient for the detection of mass anomalies below the Stickney crater, as well as large scale heterogeneous regions within plausible rubble-pile structures. Libration helps retrieve the more degenerate models for gravity, such as those with concentric layers or with density varying linearly with depth. The incremental improvement from further adding a hypothetical mean obliquity measurement is marginal. Finally, we apply the level-set inversion and the analytical formulas to estimate possible interior characteristics of the ‘real’ Phobos from the currently-available scarce geodetic observables. The level-set solutions for the real-data inversion generally converge to a higher mass concentration towards the surface in the equatorial region. Markov chain Monte Carlo estimations of parameters relative to a simple 2-layer model or a radial density distribution similarly hint at a lighter region inside of Phobos.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"426 ","pages":"Article 116343"},"PeriodicalIF":2.5,"publicationDate":"2024-10-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142552053","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":"Ab initio strewn field for small asteroids impacts","authors":"Albino Carbognani ,&nbsp;Marco Fenucci ,&nbsp;Raffaele Salerno ,&nbsp;Marco Micheli","doi":"10.1016/j.icarus.2024.116345","DOIUrl":"10.1016/j.icarus.2024.116345","url":null,"abstract":"<div><div>In recent years, nine small near-Earth asteroids were discovered a few hours before the collision with the Earth: these are about one metre in diameter objects that have all disintegrated in the atmosphere, generating bright fireballs without causing damage. In some cases, several meteorites have been recovered. In cases like these, it is not always possible to triangulate the fireball generated by the asteroid’s fall to circumscribe the strewn field position. For this reason, it can be important to compute a strewn field “ab initio”, i.e. propagating the asteroid’s trajectory in the atmosphere starting from the initial conditions obtained directly from the heliocentric orbit, coupled with some reasonable hypothesis about the mean strength and the mass of the fragments to “sample” the strewn field. By adopting a simple fragmentation model coupled with a real atmospheric profile, useful results can be obtained to locate the strewn field, as we will show for the recent falls of asteroids 2024 BX1, 2023 CX1 and 2008 TC3. It was possible to locate the strewn field of our study cases with an uncertainty of the order of one kilometre with the mean strength in the range 0.5–5 MPa and the mass of the possible final fragments in the 1 g–1 kg range. We have also verified that a pancake phase after fragmentation is unnecessary to locate the strewn field for a small asteroid fall.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"425 ","pages":"Article 116345"},"PeriodicalIF":2.5,"publicationDate":"2024-10-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142539241","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":"Rare earth element assessment in Jezero crater using the Planetary Instrument for X-ray Lithochemistry on the Mars 2020 rover Perseverance: A case study of cerium","authors":"S.J. VanBommel ,&nbsp;S. Sharma ,&nbsp;T.V. Kizovski ,&nbsp;C.M. Heirwegh ,&nbsp;J.R. Christian ,&nbsp;A.L. Knight ,&nbsp;B. Ganly ,&nbsp;A.C. Allwood ,&nbsp;J.A. Hurowitz ,&nbsp;M.M. Tice ,&nbsp;M.L. Cable ,&nbsp;W.T. Elam ,&nbsp;M.W.M. Jones ,&nbsp;B.C. Clark ,&nbsp;A.H. Treiman ,&nbsp;M.E. Schmidt ,&nbsp;Y. Liu ,&nbsp;A. Das","doi":"10.1016/j.icarus.2024.116355","DOIUrl":"10.1016/j.icarus.2024.116355","url":null,"abstract":"<div><div>The “Planetary Instrument for X-ray Lithochemistry” (PIXL) X-ray spectrometer conducts in situ geochemical analyses of martian rocks and regolith interrogated by the Mars 2020 rover, <em>Perseverance</em>. In addition to quantifying primary rock-forming elements, PIXL can quantify trace elements that in turn can provide additional constraints on the geologic history of Mars. Accurate quantifications of trace elements can require additional analytical techniques to mitigate experimental, background, and crystalline effects within PIXL spectra. In this study, we focus on reducing the impact of these effects and investigate the potential presence of rare earth elements (REEs). The study specifically investigates cerium given its typical relative abundance in many geologic materials compared to other REEs and its potential to mimic fluorescence features produced by organics under deep UV excitation. A detailed analysis of PIXL targets analyzed through the first 887 martian days of the <em>Perseverance</em> mission did not produce any conclusive Ce detections. Phosphorus-enriched materials analyzed by PIXL are estimated to contain sub-675 ppm Ce and sulfate-enriched materials sub-450 ppm Ce. The method presented can help constrain limits on the abundance of additional trace elements of interest that also face a similar analytical burden. PIXL's potential to assess REE abundances, outside of yttrium, is limited for expected concentrations in surface materials. Determining most REE concentrations in materials interrogated by <em>Perseverance</em> will therefore likely require terrestrial analyses.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"425 ","pages":"Article 116355"},"PeriodicalIF":2.5,"publicationDate":"2024-10-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142539239","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Density of Uranus moons: Evidence for ice/rock fractionation during planetary accretion","authors":"Bruno Reynard ,&nbsp;Christophe Sotin","doi":"10.1016/j.icarus.2024.116354","DOIUrl":"10.1016/j.icarus.2024.116354","url":null,"abstract":"<div><div>Current models suggest the five regular moons of Uranus formed in a single stage from a primary planetary disk or a secondary impact disk. Using latest estimates of moon masses (Jacobson, 2014), we find a power-law relationship between size and density of the moons due to varying rock/ice ratios caused by fractionation processes. This relationship is better explained by mild enrichment of rock with respect to ice in the solids that aggregate to form the moons following Rayleigh law for distillation (Rayleigh, 1896) than by differential diffusion in the disk, although the two mechanisms are not exclusive. Rayleigh fractionation requires that moon composition and density reflect their order of formation in a closed-system circumplanetary disk. For Uranus, the largest and densest moons Titania and Oberon (R ∼ 788 and 761 km, respectively) first formed, then the mid-sized Umbriel and Ariel (585 and 579 km), satellites in each pair forming simultaneously with similar composition, and finally the small rock-depleted Miranda (236 km). Fractionation likely occurred through impact vaporization during planetesimal accretion. This mechanism would add to those affecting the composition of accreting planets and moons in disks such as temporal/spatial variation of disk composition due to temperature gradients, advection, and large impacts. In the outer solar nebula, Rayleigh fractionation may account for the separation of a rock-dominated reservoir, and an ice-dominated reservoir, currently represented by CI carbonaceous chondrite/type-C asteroids and comets, respectively. Potential consequences for Uranus moons' composition are discussed.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"425 ","pages":"Article 116354"},"PeriodicalIF":2.5,"publicationDate":"2024-10-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142539456","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}