Planetary and Space Science最新文献

{"title":"Testing the binarity of asteroid (720) Bohlinia using lightcurve analysis","authors":"Denis L. Gorshanov,&nbsp;Iraida A. Sokova,&nbsp;Svetlana N. Petrova,&nbsp;Konstantin N. Naumov,&nbsp;Amir Kh. Aliev","doi":"10.1016/j.pss.2025.106217","DOIUrl":"10.1016/j.pss.2025.106217","url":null,"abstract":"<div><div>A program of observations of asteroids suspected of being binary has been launched at the Pulkovo Observatory in order to search for features inherent in binary asteroids in their lightcurves. The first asteroid observed was asteroid (720) Bohlinia. The following results were obtained from observations performed in September–October 2024. The rotation period of the asteroid (its main component) was confirmed: <em>P =</em> 8.9183 ± 0.0016 h. A decrease in brightness was detected in five segments, which can be interpreted as a result of mutual phenomena (eclipses and occultations) of the primary and secondary components. The recurrence period of the phenomena (the orbital period of the asteroid's satellite) is 17.418 ± 0.006 or 34.836 ± 0.008 h. In the segments of the lightcurve located outside the supposed mutual phenomena, brightness variations were detected, presumably caused by the axial rotation of the satellite with a period of <em>P</em>_Sat = 1.932 ± 0.003 h. Taking into account the above values obtained from the observations, a numerical model of the binary system was constructed. The selection of its parameters showed that ten variants of the set of parameters are possible, satisfying the observational data: ratio of the sizes of the components, the satellite's orbital period, its orbital inclination (±14°, ±18°, ±21°), the direction of revolution relative to the rotation of the main component and the type of observed mutual phenomena (frontal or back. A forecast was made of the time intervals in which mutual phenomena in the system of components of the asteroid should be expected in the upcoming period of its observability (September–December 2025).</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"269 ","pages":"Article 106217"},"PeriodicalIF":1.7,"publicationDate":"2025-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145621252","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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 alternative perspective on the nature of sulfur isotopic variability measured in Chang'e 5 glass beads”","authors":"James W. Dottin III","doi":"10.1016/j.pss.2025.106219","DOIUrl":"10.1016/j.pss.2025.106219","url":null,"abstract":"<div><div>Using in-situ sulfur isotope measurements of glass beads from a Chang'e 5 lunar soil, Wang et al. (2024) argue that volcanism on the moon persisted until 120 Ma. This study critically evaluates their argument using current knowledge of in-situ measurement practices and the existing literature on S-isotope fraction mechanisms. This study argues that the sulfur isotope data used as a mechanism for identifying impact glass beads versus volcanic glass beads was collected and interpreted improperly, while further failing to consider plausible alternative hypotheses. The largest fractionations in the “impact” glass beads could represent mixing with background sulfur in the instrument rather than S loss during impacts. The fractionation among the “volcanic” glass beads may be an issue of instrumental mass fractionation corrections from improper standardization or a previously unidentified lunar sulfur reservoir, rather than S loss during lunar volcanism.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"269 ","pages":"Article 106219"},"PeriodicalIF":1.7,"publicationDate":"2025-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145621253","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Site selection and thermal model for a Mars habitat built from inflatable components in the Valles Marineris region","authors":"Norbert I. Kömle ,&nbsp;Thomas Herzig ,&nbsp;Wolfgang Macher ,&nbsp;Philipp Gläser ,&nbsp;Gabor Bihari","doi":"10.1016/j.pss.2025.106216","DOIUrl":"10.1016/j.pss.2025.106216","url":null,"abstract":"<div><div>Concepts for habitats suitable for housing humans safely in an extraterrestrial environment have been presented and discussed in the literature since the begin of the space age. Aside of the Moon, human settlements on the surface of Mars move more and more into the focus of interest of space agencies and private companies. These efforts have got a large boost since the recent discoveries by the Mars probes Mars Express and ExoMars–TGO (Trace Gas Orbiter) saying that abundant water resources in the form of ice exist not only at high latitudes, but also in the much warmer equatorial regions. In particular, at the ground of the giant canyon system <em>Valles Marineris</em> they were found even close to the planetary surface and thus would be accessible for use as water supply for a Mars research station inhabited by humans. Therefore, the <em>Valles Marineris</em> region has been suggested as an optimal site for building the first human outpost on Mars, which hopefully will be realized over the coming decades. In view of this expectation, in this paper we describe a new design for a Mars habitat consisting mainly of flexible, inflatable elements including greenhouses for self-sustaining food production, in order to allow for long term residence of humans. We investigate in detail, which sites in the <em>Valles Marineris</em> region would be best suited w.r.t. solar illumination and closeness to water resources and simulate the expected temperature conditions inside the habitat during day and night periods and in different seasons. Additionally, we discuss the influence of dust storms on the living conditions inside the habitat. Note that the main focus of the presented study is on solar irradiation and heat transfer modelling, while for material research, greenhouse gardening and recycling, cosmic radiation hazards and other health and safety aspects associated with the building and maintenance of a human Mars base, we refer to other work published in the literature as well as to our own investigations carried out for a lunar habitat (<span><span>Herzig et al., 2022a</span></span>) and (<span><span>Herzig et al., 2022b</span></span>).</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"269 ","pages":"Article 106216"},"PeriodicalIF":1.7,"publicationDate":"2025-11-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145526703","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"PISCES: Plumes and Ices Simulation chamber for Enceladus and other moonS","authors":"Yaël R.A. Bourgeois,&nbsp;Stéphanie M. Cazaux","doi":"10.1016/j.pss.2025.106206","DOIUrl":"10.1016/j.pss.2025.106206","url":null,"abstract":"<div><div>The discovery of vast subsurface oceans beneath the thick ice crusts of icy moons in our Solar System has ignited global interest in their potential habitability and in the processes shaping these celestial bodies. With upcoming missions set to explore the Galilean and Cronian moons in the coming decades, experimental studies are essential for optimising mission planning, selecting and testing scientific instruments, and maximising the scientific return from future observations. In this paper, we present the Plumes and Ices Simulation Chamber for Enceladus and other moonS (PISCES) — a novel experimental setup designed to replicate the extreme environmental conditions of icy moons, with pressures reaching down to 3 × 10⁻⁵ mbar and temperatures as low as 80 K. PISCES enables controlled laboratory investigations of plume dynamics and surface interactions using a suite of integrated sensors and instruments. We describe the vacuum chamber setup, its capabilities, and its adaptability to various experimental configurations. To demonstrate its potential, we detail experiments simulating Enceladus’ plume activity with the Crevasse Laboratory Analogues for Moons (CLAM), an experimental apparatus employing 3D-printed cylindrical channels positioned above a liquid water reservoir within the vacuum chamber. This approach allows us to examine plume behaviour — including vent velocity, temperature, and particle size — in relation to subsurface conditions such as wall temperature, conduit dimensions, and expansion ratios. Ultimately, PISCES provides a groundbreaking platform for experimentally reproducing icy plumes under conditions analogous to those on Enceladus, advancing our understanding of plume physics and informing future planetary exploration efforts.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"269 ","pages":"Article 106206"},"PeriodicalIF":1.7,"publicationDate":"2025-10-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145425398","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Properties of Earth’s bow shock at large geocentric distances: A case study","authors":"Hadi Madanian ,&nbsp;Daniel B. Graham ,&nbsp;Ahmad Lalti","doi":"10.1016/j.pss.2025.106214","DOIUrl":"10.1016/j.pss.2025.106214","url":null,"abstract":"<div><div>In this study we report our analysis of rare observations of Earth’s bow shock motion at sunward geocentric distances as far as 24 Earth radii (R_E). We analyze observations from solar wind monitors and two spacecraft constellations on the dayside geospace made during a period of low Mach number and low <span><math><mi>β</mi></math></span> solar wind conditions associated with a magnetic cloud flux rope of an interplanetary coronal mass ejection (ICME). It is shown that during this period the bow shock standoff distance under these conditions is underestimated by empirical model predictions. The bow shock motion is rather asymmetric, in that the bow shock expansion in the solar wind at <span><math><mo>∼</mo></math></span>120 km/s is much faster than when it recedes at <span><math><mo>∼</mo></math></span>14 km/s. It is shown that such an asymmetric motion is driven in part by magnetosheath conditions immediately downstream of the bow shock. As the bow shock expands in the upstream solar wind, heating and deceleration of the solar wind plasma is much more effective due to a higher cross shock electrostatic potential and gyrokinetic effects. These observations are also supported by a numerical model. Further downstream of the bow shock in the magnetosheath, the plasma flow exhibits significant slowdown as a result of the fast outward propagation of the bow shock and further plasma compression.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"269 ","pages":"Article 106214"},"PeriodicalIF":1.7,"publicationDate":"2025-10-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145475485","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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 large Eddy simulation of dust-devil-like vortices on Mars: Characteristics of formation and structure","authors":"Kun Zhang ,&nbsp;Kim-Chiu Chow ,&nbsp;Kwing L. Chan ,&nbsp;Jing Xiao ,&nbsp;Tao Cai","doi":"10.1016/j.pss.2025.106215","DOIUrl":"10.1016/j.pss.2025.106215","url":null,"abstract":"<div><div>Dust devils are small, intense, and short-lived atmospheric vortices which frequently occur on Mars. In this study, a large number of dust-devil-like vortices (referred as dust devils hereafter) have been simulated by using a computational fluid dynamics model with the approach of Large Eddy Simulation (LES). When a uniform and constant heat flux is applied at the surface of the model domain, a number of dust devils appear with cyclonic or anticyclonic rotation, and the total number increases with the magnitude of the heat flux. The simulated dust devils are not randomly distributed, but generally occur at the boundary of the relatively large convection cells. With the high-resolution large eddy simulation, the structure of the dust devils is also revealed, with warm and low-pressure features in the core region.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"269 ","pages":"Article 106215"},"PeriodicalIF":1.7,"publicationDate":"2025-10-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145369821","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Low frequency electrostatic wave dynamics in the subsolar magnetosheath of Venus: A theoretical framework with multi-ion and suprathermal electrons","authors":"Adil Murad ,&nbsp;Muhammad Adnan ,&nbsp;Shahida Parveen ,&nbsp;Ikramullah ,&nbsp;Fida Younus Khattak","doi":"10.1016/j.pss.2025.106205","DOIUrl":"10.1016/j.pss.2025.106205","url":null,"abstract":"&lt;div&gt;&lt;div&gt;The propagation characteristics of low-frequency electrostatic waves are investigated in the magnetized plasma environment of Venus, where both ion cyclotron and ion acoustic modes are examined. The plasma is modeled as a four-component system composed of solar wind electrons, Venus-origin hydrogen (H&lt;span&gt;&lt;math&gt;&lt;msup&gt;&lt;mrow&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;+&lt;/mo&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/math&gt;&lt;/span&gt;), Venus-origin oxygen (O&lt;span&gt;&lt;math&gt;&lt;msup&gt;&lt;mrow&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;+&lt;/mo&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/math&gt;&lt;/span&gt;), and solar wind protons (SWP). The electrons are assumed to follow a superthermal &lt;span&gt;&lt;math&gt;&lt;mi&gt;κ&lt;/mi&gt;&lt;/math&gt;&lt;/span&gt;-distribution, consistent with spacecraft observations indicating the presence of suprathermal electrons in the Venus ionosheath. Ions are treated as warm fluids, and the analysis includes the effects of an induced magnetic field through the Lorentz force. The low-frequency approximation is justified by the dominance of electrostatic structures and slow wave dynamics near the subsolar region of Venus, as observed in Pioneer Venus Orbiter (PVO) and Venus Express (VEX) missions. This approximation allows neglecting high-frequency electromagnetic components and focusing on the electrostatic behavior critical to understanding plasma transport and wave–particle interactions in the ionosheath.&lt;/div&gt;&lt;div&gt;A general dispersion relation is derived, solved numerically, and decoupled to reveal three ion cyclotron roots and three ion acoustic roots, each associated with the different ion species. In the nonlinear regime, a Zakharov–Kuznetsov (ZK) equation is derived using reductive perturbation theory to describe the evolution of small but finite-amplitude ion acoustic solitons. The analysis shows that superthermality significantly affects soliton properties: for hydrogen acoustic modes, low &lt;span&gt;&lt;math&gt;&lt;mi&gt;κ&lt;/mi&gt;&lt;/math&gt;&lt;/span&gt; values yield rarefactiolitons while higher &lt;span&gt;&lt;math&gt;&lt;mi&gt;κ&lt;/mi&gt;&lt;/math&gt;&lt;/span&gt; values support compressive structures, indicating a polarity switch linked to suprathermal electronve s populations. The amplitude and width of the solitons are further influenced by the magnetic field and solar wind proton density—higher field strength reduces width due to enhanced dispersive effects, while increased proton density decreases amplitude in oxygen modes but increases it in hydrogen modes.&lt;/div&gt;&lt;div&gt;A two-dimensional pulse stability analysis based on the Allen–Rowlands method reveals that both magnetic field and solar wind proton density suppress the first-order instability growth rate. Second-order instability becomes significant beyond the critical propagation angle (&lt;span&gt;&lt;math&gt;&lt;mrow&gt;&lt;mi&gt;θ&lt;/mi&gt;&lt;mo&gt;&gt;&lt;/mo&gt;&lt;mn&gt;37&lt;/mn&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;msup&gt;&lt;mrow&gt;&lt;mn&gt;8&lt;/mn&gt;&lt;/mrow&gt;&lt;mrow&gt;&lt;mo&gt;∘&lt;/mo&gt;&lt;/mrow&gt;&lt;/msup&gt;&lt;/mrow&gt;&lt;/math&gt;&lt;/span&gt;), particularly for proton modes. These results align with observed electrostatic wave behavior and density fluctuations reported in PVO and VEX datasets, highlighting the role of multi-ion interactions and suprathermal effects in shaping Venus","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"268 ","pages":"Article 106205"},"PeriodicalIF":1.7,"publicationDate":"2025-10-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145324423","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Orbital geomorphological mapping of Jezero Crater and comparative insights from Gale Crater","authors":"Fatima-Ezzahra Jadid ,&nbsp;Hasnaa Chennaoui Aoudjehane ,&nbsp;Cristian Carli ,&nbsp;Beatrice Baschetti ,&nbsp;Riccardo Pozzobon","doi":"10.1016/j.pss.2025.106207","DOIUrl":"10.1016/j.pss.2025.106207","url":null,"abstract":"<div><div>Understanding the geomorphology of ancient Martian Lake systems is crucial for unraveling the planet's past climate and potential habitability. This study addresses persistent gaps in basin-scale mapping by presenting the first comprehensive, high-resolution (1:25,000 scale) geomorphological map of Jezero Crater, produced from integrated CTX and HiRISE orbital datasets. The new map covers the entire crater, including previously underexplored eastern sectors, and highlights spatial relationships among fractured floor units, delta deposits, and crater rim features. These results offer new insights into the geological processes that shaped the basin.</div><div>To broaden the planetary context, we also revisited previous mapping efforts on Gale Crater and compared them with Jezero. Building on previous work, we refine Gale's geomorphological framework by incorporating additional features, enabling a crater-wide comparative synthesis of fluvial histories. Both sites were mapped using a consistent methodology and well-defined dataset selection criteria.</div><div>Our results demonstrate that Jezero experienced longer-lasting and more stable fluvial activity than Gale, highlighting the diversity of local hydrological regimes during Mars's transition from wetter to drier climates. This integrated approach advances the geomorphological context needed for interpreting in situ rover data and for guiding future exploration, and it provides a robust foundation for reconstructing early Martian paleoenvironments.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"268 ","pages":"Article 106207"},"PeriodicalIF":1.7,"publicationDate":"2025-10-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145324422","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Decoding the Apollo basin: Insights into volcanism, compositional diversity and crustal evolution","authors":"C.R. Neeraja,&nbsp;S Arivazhagan,&nbsp;P Abishek","doi":"10.1016/j.pss.2025.106204","DOIUrl":"10.1016/j.pss.2025.106204","url":null,"abstract":"<div><div>The Apollo basin, within the South Pole-Aitken (SPA) basin on the far side of the Moon, is a notable geological feature that offers an understanding of the Moon's history and evolution and showcases a complex geological history influenced by impact processes and volcanic activity. The present study focused on delineating the basaltic flows of the basin along with age determination and lithological discrimination. The current research utilized Chandrayaan-1 Moon Mineralogy Mapper (M³), Chandrayaan-2 Imaging Infra-Red Spectrometer (IIRS), Lunar Reconnaissance Orbiter Camera (LROC) - Wide Angle Camera (WAC), Kaguya Terrain Camera (TC) and Kaguya Multiband Imager (MI) derived maps. The FeO weight percent map, Mg # map generated from Kaguya MI data, and the TiO₂ abundance map from LROC WAC data are used for the compositional analysis. The mare is classified into eight distinct units by comparing these parameters with an Integrated Band Depth (IBD) color composite image. Spectral studies are done to identify the pyroxene mineralogy of each unit. By analyzing the pyroxene thermometry plot generated by analyzing the spectral data, two distinct crystallization trends are observed, starting with pigeonite and sub-calcic augite to ferro-augite. The other trend progresses from augite to diopside boundary. The ages of the mare units were estimated using the Crater Size Frequency Distribution (CSFD) method. The study suggests that mare volcanism commenced at approximately 3.5 Ga and progressed to a younger phase between 2.0 and 1.8 Ga. The units A2 and A4 exhibit the highest average model age (AMA) of 3.5 Ga and dominantly exhibit higher calcium content, while unit A8 represents the youngest unit with an age of 1.8 Ga with relatively lower calcium content. Mare volcanism was initiated at the periphery of the basin, particularly in the southern and southeastern regions, and subsequently progressed westward and towards the basin's center. Magmas with diverse chemical compositions derived from varied source regions erupted in the Apollo basin between the Imbrian and Eratosthenian periods.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"268 ","pages":"Article 106204"},"PeriodicalIF":1.7,"publicationDate":"2025-10-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145324421","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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 chemistry and mineralogy of the LX high-fidelity lunar regolith simulants","authors":"Joel Patzwald ,&nbsp;Ferry Schiperski ,&nbsp;Hannah Fisher ,&nbsp;Thomas Neumann ,&nbsp;Enrico Stoll","doi":"10.1016/j.pss.2025.106190","DOIUrl":"10.1016/j.pss.2025.106190","url":null,"abstract":"<div><div>To support sustainable solar system exploration, humans must harness resources from celestial bodies like the Moon to build infrastructure and obtain essential consumables, including water and oxygen. Lunar regolith, a loose rock layer covering the Moon’s surface, is a key resource for in-situ resource utilisation (ISRU) technologies. Developing and testing these technologies on Earth relies on the use of accurate simulant materials. In prior studies, the LX lunar regolith simulant system was developed and the base simulants LX-T100 (anorthosite) and LX-M100 (basalt) were thoroughly characterised in terms of their bulk mineralogical and bulk chemical composition, particle size distribution, particle morphology, density, void ratio and porosity, adsorption and BET-specific surface area, compressibility, flow, magnetic and optical properties. This work focuses on the LX high-fidelity simulants, specifically their mineralogy and chemistry. The high-fidelity simulants are composed of four source rocks, namely the anorthosite of LX-T100, the basalt of LX-M100, as well as a harzburgite as a source for olivine and pyroxene and an ilmenite ore as a source for ilmenite. The bulk mineralogy and chemistry of the harzburgite and ilmenite ore, as well as the crystal chemistry of all four source rocks, were analysed and the results were compared with the lunar samples from the Apollo and Luna missions. Finally, a deviation analysis was carried out in which the bulk chemistry of the LX high-fidelity simulants and 13 other relevant simulants from research and industry were compared with the chemical composition of the lunar soil at the landing sites of the Apollo, Luna and Chang’e 5 missions. It was shown that of all simulants, the LX high-fidelity simulants can on average best mimic the chemical composition of the lunar soil. The findings from these investigations deepen the understanding of the LX lunar regolith simulants, increasing their reliability for scientific research.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"268 ","pages":"Article 106190"},"PeriodicalIF":1.7,"publicationDate":"2025-09-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145220428","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}