Icarus最新文献

{"title":"A Pyroxenite mantle on Mercury? Experimental insights from enstatite chondrite melting at pressures up to 5 GPa","authors":"Asmaa Boujibar , Kevin Righter , Emmanuel Fontaine , Max Collinet , Sarah Lambart , Larry R. Nittler , Kellye M. Pando","doi":"10.1016/j.icarus.2025.116602","DOIUrl":"10.1016/j.icarus.2025.116602","url":null,"abstract":"<div><div>Enstatite chondrites are potential source material for the accretion of Mercury due to their reduced nature and enrichment in volatile elements. Understanding their melting properties is therefore important to better assess a scenario where Mercury formed from these chondrites. Here, we present experimental data on the partial melting of a modified EH4 Indarch enstatite chondrite, which was adjusted to have 18 % more metallic Si than SiO<sub>2</sub> in mass, yielding an oxygen fugacity of 3.7 ± 0.6 below iron-wüstite redox buffer and 12 wt% Si in the metal. Experiments were performed from 0.5 to 5 GPa using piston cylinder and multi-anvil apparatuses. Results indicate that the stability field of enstatite expands relative to olivine. This expansion is likely due to the presence of Ca-S and Mg-S complexes in the silicate melt, which enhance SiO<sub>2</sub> activity and promote enstatite crystallization. Silicate melts present a correlation between Ca and S concentrations, like the global patterns seen on Mercury's surface but with higher sulfur abundances. Additionally, sulfides show enrichment in Mg and Ca, up to 22 and 13 wt% respectively, the main remaining cations being Fe, Cr and Mn. These high Mg and Ca contents are observed at low temperatures and high silica content in the silicate melt, respectively. Partial melting of this reduced EH4 chondrite yields a large range of silicate melt compositions, due to the Mg- and Ca-rich sulfides which act as significant residual phases. High-pressure melts (2 to 5 GPa, 160–400 km depth in Mercury) are Mg-rich, similar to those in Mercury's high‑magnesium region (HMR), while low-pressure melts (0.5 to 1 GPa, 40–80 km depth) are Si-rich, comparable to the northern volcanic plains (NVP). Results suggest that a large fraction of Mercury's surface aligns compositionally with these melts, implying that Mercury's mantle could predominantly have a pyroxenitic composition. However, regions with differing compositions, such as aluminum-rich areas, like the Caloris basin, suggest local variability in mantle geochemistry. The HMR chemistry indicates melting at pressures up to the base of Mercury's mantle, possibly due to a large impact. Our study also explores whether the surface compositions could result from mixing processes like impact gardening or polybaric melting and magma mixing. The findings suggest that areas such as the intercrater plains and heavily cratered regions could be mixtures of melts from different pressures, ranging from 0.5 to 5 GPa, which corresponds to the crust-mantle to core-mantle boundaries. Overall, our results show that if Mercury formed from materials similar to enstatite chondrites, batch melting of its primitive pyroxenite mantle would yield magmas with compositions resembling those of most rocks observed on the surface. While the exact olivine content of the mantle remains uncertain, the residual mantle is likely enstatite-rich due to the extensive stability of enstatite","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"437 ","pages":"Article 116602"},"PeriodicalIF":2.5,"publicationDate":"2025-04-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143859478","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":"A highly resonant Neptunian region: A systematic search for two-body and three-body mean-motion resonances","authors":"Evgeny Smirnov","doi":"10.1016/j.icarus.2025.116584","DOIUrl":"10.1016/j.icarus.2025.116584","url":null,"abstract":"<div><div>In this study, a large-scale numerical investigation of resonant objects in the Neptune region is presented, focusing on both two-body and three-body mean-motion resonances (MMRs). Two separate simulations were conducted to identify resonant populations and quantify their prevalence.</div><div>In Simulation 1, two-body MMRs with Uranus and Neptune up to the resonant order <span><math><mrow><mi>q</mi><mo>≤</mo><mn>10</mn></mrow></math></span>, as well as three-body MMRs involving both planets up to the order <span><math><mrow><mi>q</mi><mo>≤</mo><mn>6</mn></mrow></math></span>, were examined. Using automated resonance classification techniques, it was found that 42.1% of objects are resonant, increasing to 58.2% when including controversial cases. This is significantly higher than the resonant fraction observed in the main asteroid belt. The results confirm that two-body MMRs with Neptune dominate, with a smaller but significant fraction of three-body resonances and two-body resonances with Uranus.</div><div>In Simulation 2, the analysis was extended to higher-order (<span><math><mrow><mi>q</mi><mo>≤</mo><mn>20</mn></mrow></math></span>) and high-integer-coefficient (<span><math><mrow><msub><mrow><mi>m</mi></mrow><mrow><mi>i</mi></mrow></msub><mo>≤</mo><mn>50</mn></mrow></math></span>) two-body resonances with Neptune, testing whether previously classified non-resonant objects might belong to higher-order MMRs. This second simulation revealed an additional 108 resonances and 104 new confirmed resonant objects, bringing the total fraction of resonant asteroids in the region to 49.3% confirmed cases and 65.1% with controversial cases included. Many new two-body MMRs with Neptune are found. Notably, some objects were found to be trapped in multiple resonances simultaneously.</div><div>These results demonstrate that MMRs play an important role in shaping the trans-Neptunian region, with an overall resonance fraction more than three times higher than in the main asteroid belt. All objects in this region may be in fact resonant.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"436 ","pages":"Article 116584"},"PeriodicalIF":2.5,"publicationDate":"2025-04-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143815993","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":"Long-distance ranging and velocity measurements by REASON on Europa Clipper","authors":"Michelle S. Park ,&nbsp;Gregor Steinbrügge ,&nbsp;Elizabeth Wig ,&nbsp;Dustin M. Schroeder ,&nbsp;Erwan Mazarico ,&nbsp;Donald D. Blankenship","doi":"10.1016/j.icarus.2025.116585","DOIUrl":"10.1016/j.icarus.2025.116585","url":null,"abstract":"<div><div>One of the objectives of the Gravity and Radio Science (G/RS) instrument on NASA’s Europa Clipper mission is to improve our knowledge of Europa’s ephemerides, to trace the moon’s thermal-orbital evolution. Here, we present a complementary methodology to use the Radar for Europa Assessment and Sounding: Ocean to Near-surface (REASON) instrument to enhance these measurements by tracking echoes from Europa at greater distances, beyond its primary role of subsurface sounding during close flybys. We investigate the possibility of occasional REASON measurements during the non-nadir phase at altitudes beyond 40,000 km to extend the ephemerides dataset. Through radar simulations of REASON’s echoes, we evaluate and demonstrate this approach by determining the maximum altitude for surface return detection, achieved by coherently processing hundreds to thousands of pulses within the signal’s round-trip time. The received signal’s power can be further enhanced by maximizing pulse length, targeting Europa’s most reflective (leading sub-Jovian) hemisphere, and summing many compressed pulses. We also explore a phase shift approach for velocity measurements, which uses existing ranging pulses. Using Europa Clipper’s most recent trajectory design, we identify flybys that align with the best working scenarios for this approach. Our performance estimates for range and velocity resolution demonstrate that this approach could obtain measurements relevant to Europa’s ephemerides. This method offers key insights into Europa’s orbital evolution and, ultimately, its long-term habitability.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"436 ","pages":"Article 116585"},"PeriodicalIF":2.5,"publicationDate":"2025-04-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143834830","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":"Climatology of transient eddies and dust storms in the southern hemisphere of Mars","authors":"David Hinson","doi":"10.1016/j.icarus.2025.116581","DOIUrl":"10.1016/j.icarus.2025.116581","url":null,"abstract":"<div><div>This paper examines the behavior of transient eddies in the southern hemisphere of Mars and illustrates how the eddies shape the annual cycle and spatial distribution of dust storms. The investigation of transient eddies is based on off-nadir measurements of brightness temperature by the Mars Climate Sounder, which are the most direct and reliable source of information about eddy activity adjacent to the surface. Basic properties of the transient eddies are determined through least-squares analysis of brightness temperatures spanning 8.6 Mars years, yielding a far more complete description of eddy activity in the southern hemisphere than was available previously. The space-time spectrum is dominated by eddies with zonal wavenumbers 1–4 and periods shorter than 5 sols. The wave-4 component is much more important than was previously recognized. An annual cycle comprising three distinct periods of eddy activity is observed each year. Shallow (in temperature) baroclinic waves are present at <span><math><mrow><msub><mrow><mi>L</mi></mrow><mrow><mi>s</mi></mrow></msub><mo>=</mo><mn>0</mn></mrow></math></span>–<span><math><mrow><mn>75</mn><mo>°</mo></mrow></math></span> and <span><math><mrow><mn>125</mn></mrow></math></span>–<span><math><mrow><mn>200</mn><mo>°</mo></mrow></math></span>. In the intervening period, the baroclinic waves are replaced by a deep, 3.3-sol, barotropic wave that has a relatively small amplitude near the surface. The transient eddies strongly influence the annual cycle of discrete dust storms cataloged in the Mars Dust Activity Database and the Mars Dust Storm Sequence Dataset. Dust storms are rare and their net area is negligible during the barotropic phase of eddy activity (<span><math><mrow><msub><mrow><mi>L</mi></mrow><mrow><mi>s</mi></mrow></msub><mo>=</mo><mn>75</mn></mrow></math></span>–<span><math><mrow><mn>125</mn><mo>°</mo></mrow></math></span>), when the amplitude near the surface is small. Conversely, the wind stress routinely exceeds the threshold required for dust lifting during the two baroclinic phases of eddy activity, when the amplitude near the surface is much larger, resulting in a conspicuous increase in the net area of the dust storms. Dust storms occur frequently in a corridor extending from Aonia Terra to Margaritifer Terra, owing to the presence of a persistent storm track of eddy activity in the western hemisphere. The density of dust storms in this corridor varies in response to the seasonal evolution in the strength and latitude of the storm track. Further insight is gained by consolidating results from previous studies. This investigation improves our understanding of the Martian climate in the half year centered on the southern winter solstice, when the atmosphere is relatively cool and clear.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"436 ","pages":"Article 116581"},"PeriodicalIF":2.5,"publicationDate":"2025-04-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143807942","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":"Effects of observation geometry and heating on the ultra-violet to near-infrared spectra of Mercury simulant","authors":"Mireia Leon-Dasi ,&nbsp;Sebastien Besse ,&nbsp;Camille Cartier ,&nbsp;Océane Barraud ,&nbsp;Alessandro Maturilli ,&nbsp;Alain Doressoundiram ,&nbsp;Johannes Benkhoff ,&nbsp;Laurie Llado","doi":"10.1016/j.icarus.2025.116582","DOIUrl":"10.1016/j.icarus.2025.116582","url":null,"abstract":"<div><div>The temperature of Mercury varies greatly across different latitudes due to the planet’s spin/orbit resonance, leading to modifications in the surface spectral properties. The upcoming BepiColombo mission will map the surface of the planet in the UV-TIR range, providing a more comprehensive understanding of the surface alteration. However, comparing the spectral measurements between BepiColombo and the past MESSENGER mission could be challenging due to the large differences in observation geometry. Laboratory experiments with close surface analogs in viewing conditions similar to the space-based observations are necessary to understand the effect of the space environment and interpret the orbital spectral measurements. This study presents the UV-NIR spectroscopy of a Mercury simulant to understand the impact of observation geometry and temperature on the spectral properties of the planet’s surface. The simulant (a mixture of aubrites, albite, and synthetic sulfides) and its endmembers are measured under six geometries that sample the viewing conditions of both missions. The samples are measured fresh and after heating to 450 °C during three cycles. This study finds that the observation geometry modifies the reflectance spectrum of the samples differently depending on the wavelength and composition. The analog presents a darkening, reddening, and flattening with increasing phase angle in the UV-NIR domain. The heated samples present a brightening and reddening, with a deepening of absorption bands. The spectral changes associated with observation geometry and heating are stronger with increasing Mg abundance.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"436 ","pages":"Article 116582"},"PeriodicalIF":2.5,"publicationDate":"2025-04-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143807943","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":"Modelling the effect of volcanic outgassing of sulphur on early Martian surface temperatures using a 3-D Global Climate Model","authors":"A.S. Braude ,&nbsp;L. Kerber ,&nbsp;F. Lefèvre ,&nbsp;A.Y. Jaziri ,&nbsp;S.S. Hamid ,&nbsp;M. Lefèvre ,&nbsp;M. Maurice ,&nbsp;E. Millour ,&nbsp;F. Forget","doi":"10.1016/j.icarus.2025.116568","DOIUrl":"10.1016/j.icarus.2025.116568","url":null,"abstract":"<div><div>Around the time of the transition from the Late Noachian to the Early Hesperian eras (<span><math><mo>∼</mo></math></span>3.6 Gya), Mars was predicted to have been both volcanically active, and have sustained a climate warm enough to melt liquid water on its surface episodically despite a faint young sun. The effect of volcanic outgassing on the climate of early Mars and its ability to raise temperatures above the melting point of water has, however, been disputed, with a major uncertainty being the timescales over which the greenhouse effect of outgassed sulphur dioxide (SO₂) and hydrogen sulphide (H₂S) can warm the atmosphere of Mars before they react to form H₂SO₄ and S₈ aerosols which act to cool the surface of Mars. We have developed the first 3-D model of the Martian sulphur cycle from source to sink that includes outgassing of SO₂, H₂S and S₂ from the surface, the formation of H₂SO₄ and S₈ through atmospheric chemistry, and the condensation and deposition of H₂SO₄ and S₈ to the surface. We simulate the effect of a single large, day-long volcanic outgassing event on global surface temperatures, identifying the magnitude and duration of any net warming and cooling as a function of outgassing magnitude, atmospheric pressure, obliquity and aerosol particle size distribution. We confirm the results of Tian et al. (2010, EPSL 295, 412-418) and find that the persistence of the warming effect of volcanically outgassed SO₂ and H₂S on the Martian atmosphere is only of the order of days to weeks for a surface pressure range of between 0.5 and 1.5 bars. Typical outgassing magnitudes result in a net cooling of the Martian surface over timescales of 3–4 years near the equator and several decades at the poles for plume neutral buoyancy heights within the troposphere. For very high magnitudes of outgassing, the rate of H₂SO₄ cloud formation slows down due to the depletion of water vapour in the atmosphere, thereby slowing down the rate of cooling and providing a buffer against atmospheric collapse.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"436 ","pages":"Article 116568"},"PeriodicalIF":2.5,"publicationDate":"2025-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143820569","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":"Investigating grain size in the Martian mantle: Implications of basal mantle layers and viscoelastic models","authors":"Feng Liang ,&nbsp;Jianguo Yan ,&nbsp;Chi Xiao ,&nbsp;Yuji Harada ,&nbsp;Jean-Pierre Barriot","doi":"10.1016/j.icarus.2025.116592","DOIUrl":"10.1016/j.icarus.2025.116592","url":null,"abstract":"<div><div>This study examines the grain size in the Martian mantle using viscoelastic dissipation models and two interior structural configurations: S23M1 (without a basal mantle layer, BML) and S23M2 (with a BML). Results indicate substantial variations in grain size estimates depending on the viscoelastic model employed. For instance, Andrade(<em>μ-β</em>) models suggest smaller grain sizes (∼1 mm), while Burgers(background), Burgers(+peak), and Andrade(fixed <em>β</em>) models predict a broader range of 0.1–10 cm. Sundberg-Cooper models, by contrast, yield larger grain sizes (&gt;0.5 cm). The inclusion of a BML generally leads to smaller grain size estimates. For instance, Sundberg-Cooper predictions decrease from ∼10 cm to ∼0.8 cm with a BML, attributed to altered average rigidity of Mars that reduces elastic response. These findings stress the importance of mantle structure in interpreting viscoelastic properties and reconciling laboratory-derived constraints with geophysical observations. Future tidal measurements are critical for refining these models further.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"436 ","pages":"Article 116592"},"PeriodicalIF":2.5,"publicationDate":"2025-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143834829","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":"An energy-angular momentum phase function for rubble pile asteroids","authors":"D.J. Scheeres","doi":"10.1016/j.icarus.2025.116563","DOIUrl":"10.1016/j.icarus.2025.116563","url":null,"abstract":"<div><div>This work analyzes the energetics of asteroid rubble piles in order to understand what asteroid morphologies should naturally arise from their formation and evolution process. In doing this, a phase diagram is developed that maps out the range of final minimum energy states that a collapsing gravitational aggregate can achieve as a function of total angular momentum and mass distribution. This is developed assuming properties associated with rubble pile asteroids, and can provide insight into the formation and subsequent evolution of contact binaries and orbital binaries in the solar system as an outcome of catastrophic disruptions. The system angular momentum is used as an independent parameter, combined with resulting minimum energy configurations as a simple function of mass morphology of the final system. The configuration of systems with an energy boosted above the minimum energy state are also considered. This paper considers an ideal case, but outlines general results that can be continued for more precise models of distributed granular media modeled using continuum models or using discrete element models.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"436 ","pages":"Article 116563"},"PeriodicalIF":2.5,"publicationDate":"2025-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143786107","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 source of hydrogen in earth's building blocks","authors":"Thomas J. Barrett ,&nbsp;James F.J. Bryson ,&nbsp;Kalotina Geraki","doi":"10.1016/j.icarus.2025.116588","DOIUrl":"10.1016/j.icarus.2025.116588","url":null,"abstract":"<div><div>Despite being pivotal to the habitability of our planet, the process by which Earth gained its present-day hydrogen budget is unclear. Due to their isotopic similarity to terrestrial rocks across a range of elements, the meteorite group that is thought to best represent Earth's building blocks is the enstatite chondrites (ECs). Because of ECs' nominally anhydrous mineralogy, these building blocks have long been presumed to have supplied negligible hydrogen to the proto-Earth. However, recent bulk compositional measurements suggest that ECs may unexpectedly contain enough hydrogen to readily explain Earth's present-day water abundance. Together, these contradictory findings mean the contribution of ECs to Earth's hydrogen budget is currently unclear. As such, it is uncertain whether appreciable hydrogen is a systematic outcome of Earth's formation. Here, we explore the amount of hydrogen in ECs as well as the phase that may carry this element using sulfur X-ray absorption near edge structure (S-XANES) spectroscopy. We find that hydrogen bonded to sulfur is prevalent throughout the meteorite, with fine matrix containing on average almost 10 times more H<img>S than chondrule mesostasis. Moreover, the concentration of the H<img>S bond is linked to the abundance of micrometre-scale pyrrhotite (Fe_1-xS, 0 &lt; x &lt; 0.125). This sulfide can sacrificially catalyse a reaction with H₂ from the disk at high temperatures to create H₂S, which could be dissolved in adjoining molten silicate-rich material. Upon rapid cooling, this assemblage would form pyrrhotite encased in submicron silicate-rich glass that carries trapped H₂S. These findings indicate that hydrogen is present in ECs in higher concentrations than previously considered and could suggest that this element may have a systematic, rather than stochastic, origin on our planet.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"436 ","pages":"Article 116588"},"PeriodicalIF":2.5,"publicationDate":"2025-04-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143864671","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":"Asteroid phase curves and phase coloring effect using the ATLAS survey data","authors":"Milagros Colazo ,&nbsp;Dagmara Oszkiewicz ,&nbsp;Alvaro Alvarez-Candal ,&nbsp;Patrycja Poźniak ,&nbsp;Przemysław Bartczak ,&nbsp;Edyta Podlewska-Gaca","doi":"10.1016/j.icarus.2025.116577","DOIUrl":"10.1016/j.icarus.2025.116577","url":null,"abstract":"<div><div>We determined phase curves for 301<span><math><mo>,</mo></math></span>272 asteroids in the orange filter and 280<span><math><mo>,</mo></math></span>953 in the cyan filter from the latest ATLAS Solar System Catalog V2 (SSCAT-2). Among them, 3<span><math><mo>,</mo></math></span>345 and 492 asteroids in the orange and cyan filters, respectively, have uncertainties below 15%. Our simple model, which considers only the apparition effect, showed good consistency with more sophisticated methods requiring much less computational time. Database cross-matching allowed us to analyze G1 and G2 distributions according to taxonomy. We conducted two-dimensional Kolmogorov–Smirnov tests to investigate two distinct aspects: similarities in paired G1, G2 distributions across different taxa and wavelength dependency within the same taxa. When comparing different taxa, we could not reject the null hypothesis for 11% of the orange sample and 31% of the cyan sample, indicating more disparities in the orange filter. For wavelength dependency, paired distributions of G1, G2 (o) vs. G1, G2 (c) showed statistically significant differences across all complexes, except for the A class. Our analysis suggests that while phase coloring behaviors are observed without a clear preference for reddening or bluening at phase angles below 5°, reddening predominates in the 10°–30°range. We also observed smaller uncertainties in G2 than in G1. Simulations showed that G2 is less sensitive to lack of data at small phase angles. This is related to the definition of the H, G1, G2 function, where G1 contributes more to the opposition effect and G2 the linear part of the phase curve. Our catalog-independent algorithms are adaptable to new data sets, including future LSST data.</div></div>","PeriodicalId":13199,"journal":{"name":"Icarus","volume":"436 ","pages":"Article 116577"},"PeriodicalIF":2.5,"publicationDate":"2025-04-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143799738","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}