Planetary and Space Science最新文献

{"title":"Properties of novel LX lunar regolith simulant system — the base simulants: Part 2","authors":"Joel Patzwald ,&nbsp;Rafael Kleba-Ehrhardt ,&nbsp;Tjorben Griemsmann ,&nbsp;Norbert Nowaczyk ,&nbsp;Stefan Linke ,&nbsp;Ludger Overmeyer ,&nbsp;Enrico Stoll ,&nbsp;David Karl","doi":"10.1016/j.pss.2025.106189","DOIUrl":"10.1016/j.pss.2025.106189","url":null,"abstract":"<div><div>Sustainable and fast exploration and colonisation of our solar system are only possible if humans learn to use the resources of other celestial bodies, such as our Moon, to build settlements and infrastructure, extract valuable materials for the production of secondary goods and obtain consumables such as water and oxygen for life support and as fuel. The most abundant resource on the Moon is the lunar regolith, a layer of loose pulverised rock material covering the Moons surface many meters thick. So-called ISRU (in-situ resource utilisation) technologies are being developed to make use of this material. To develop and test such technologies on Earth, analogue materials (simulants) are essential. In a previous study, the LX lunar regolith simulant system was developed for this purpose, and the base simulants LX-T100 and LX-M100 were characterised regarding their mineralogy and chemistry, particle size distribution, particle morphology, density, void ratio and porosity. This study presents the second part of a comprehensive characterisation of the base simulants, aimed at providing detailed insights into their adsorption behaviour and specific surface area, compressibility, flow properties, magnetic properties and optical properties. Using the Brunauer–Emmett–Teller (BET) method, the specific surface area was precisely quantified, being, for example, relevant to the adhesion and reactivity of lunar dust. Compressibility was measured using an oedometer test, providing insight into the settlement behaviour of the simulants under load. Flow properties were assessed through a series of dynamic and static tests, including angle of repose, Hausner ratio, rheometry and direct shear measurements, to determine the simulant’s handling and transportation behaviour. The magnetic properties were characterised to understand the magnetic susceptibility and remanence, which are crucial for dust mitigation strategies and electromagnetic interference assessments. Spectral reflectance was evaluated using spectrophotometry across relevant wavelengths, providing useful data for remote sensing calibration and surface composition analysis. It was shown that the simulants are good analogues for simulating adsorption, compression, and flow behaviour. However, their ability to represent magnetic and optical properties remains limited. The results from these investigations contribute to a more thorough understanding of the LX base simulants, enhancing their fidelity for scientific research.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"268 ","pages":"Article 106189"},"PeriodicalIF":1.7,"publicationDate":"2025-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145020372","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":"2025-11-15","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}

{"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":"2025-11-15","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":"MICROorganisms under simulated ICY moon environments: supporting solar system exploration (MICRO ICY project)","authors":"C. Pacelli ,&nbsp;A. Cassaro ,&nbsp;L. Cocola ,&nbsp;A. Cordone ,&nbsp;M. Del Bianco ,&nbsp;M. Esposito ,&nbsp;F. Ferranti ,&nbsp;M. Ferrara ,&nbsp;D. Giovannelli ,&nbsp;L. Manfrin ,&nbsp;L. Parca ,&nbsp;L. Poletto ,&nbsp;L. Tonietti ,&nbsp;A. Zinzi","doi":"10.1016/j.pss.2025.106200","DOIUrl":"10.1016/j.pss.2025.106200","url":null,"abstract":"<div><div>The exploration of icy moons in the solar system marks a new chapter in the search for extraterrestrial life, with next-generation missions targeting these promising environments. Cassini's flybys of Enceladus revealed a global subsurface ocean containing organic compounds and biologically available nitrogen, suggesting potential conditions for life as we know it. Other moons with subsurface oceans, such as Europa, Titan, Ganymede, and Callisto, are now considered more common in the cosmos than once believed. Enceladus thus provides a critical platform for advancing astrobiological research and technology.</div><div>Given the challenges of space exploration, Earth-based (both in-situ and laboratory) experiments are crucial for interpreting remote data and understanding icy moon processes. Terrestrial hydrothermal sites, similar to those expected on Enceladus, shed light on the origins and preservation of life, expanding our knowledge of the habitability concept. Microbial extremophiles thriving in these environments allow to refine life's boundaries and support the search for life elsewhere.</div><div>In this context, the MICROICY project aims to: (i) study microbial communities in the Strýtan alkaline shallow-water hydrothermal vents in Iceland, analogues to Enceladus' hydrothermal vents; (ii) assess the adaptation mechanisms of extremophiles under Enceladus-like conditions; and (iii) detect gas biosignatures of microbial activity using a mass spectrometry detector. These findings will support the use of gas biosignatures in next-generation astrobiology missions, advancing the exploration of Enceladus and other icy moons.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"268 ","pages":"Article 106200"},"PeriodicalIF":1.7,"publicationDate":"2025-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145106174","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":"Secondary electron generation by sub-keV ion and energetic neutral particle impacts on a surface","authors":"S. Gopalakrishnan,&nbsp;X. Wang,&nbsp;H.-W. Hsu,&nbsp;M. Horányi","doi":"10.1016/j.pss.2025.106202","DOIUrl":"10.1016/j.pss.2025.106202","url":null,"abstract":"<div><div>The secondary electron yield (SEY) from sub-keV ion and neutral particle impacts on a stainless steel surface has been investigated in the laboratory. Sub-keV ions were generated using a large Kauffman ion source and energetic neutral particles (ENPs) were generated from ion-neutral charge-exchange collisions. It is found that the SEY from ion impacts increases with the ion kinetic energy, reaching the yield of <span><math><mo>∼</mo></math></span>0.25-0.4 by the 1000 eV ion impact, depending on the surface cleanliness. The SEY from neutral impacts is about an order of magnitude lower than from ion impacts, indicating that the electrostatic potential energy plays a bigger role in generating secondary electrons than the kinetic energy in this energy range. It is shown that the SEY is higher for impacts by lighter ion species. The effect of surface cleanliness is investigated, showing an increase in the SEY for a contaminated surface. Our results show that secondary electrons generated from sub-keV ion impacts are non-negligible and may play a more pronounced role in determining the surface charge in various space environments, such as permanently shadowed regions (PSRs) on airless bodies. The SEY measured from sub-keV ENP impacts is useful for determining the surface charge of a spacecraft moving through dense planetary atmospheres.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"268 ","pages":"Article 106202"},"PeriodicalIF":1.7,"publicationDate":"2025-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145158459","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":"Nonlinear theory of dust-acoustic waves in planetary plasmas with non-ideal dust fraction","authors":"Alexander E. Dubinov,&nbsp;Ilya N. Kitayev","doi":"10.1016/j.pss.2025.106199","DOIUrl":"10.1016/j.pss.2025.106199","url":null,"abstract":"<div><div>A non-ideal dusty planetary plasma was considered, consisting of a mixture of three gases – gases of inertialess electrons and ions, and a gas of negatively charged dust particles. Electrons and ions in the plasma were thought to be Boltzmann-distributed, and the dust gas obeyed the equation of state of the non-ideal gas previously deduced by Avinash. Stationary dust-acoustic waves DAWs in such plasma were studied for the first time. The study was carried out in the gas dynamic approach.</div><div>The linear theory of DAWs has been developed, within the framework of which a dispersion equation was derived and an exact expression for the linear velocity of a dust sound was obtained.</div><div>The non-linear theory of large amplitude DAWs in a non-ideal dust plasma based on the Bernoulli pseudopotential method was first developed. Pseudopotential analysis showed that stationary DAWs in the considered plasma can have the form of either a nonlinear periodic wave or the form of solitons. The wave velocity ranges in these two forms are defined.</div><div>The dependence of the maximum velocity of DA-solitons and the maximum Mach number on the value of the parameter of non-ideality is calculated. It was also found that with an increase of the parameter of non-ideality, the amplitude of the extreme soliton decreases, and its width at half-maximum practically does not depend on this parameter.</div><div>The developed theory can be used to describe DAWs appearing in dense non-ideal plasmas near planets, their satellites and comets.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"268 ","pages":"Article 106199"},"PeriodicalIF":1.7,"publicationDate":"2025-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145057159","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":"Comparison of Kelvin–Helmholtz waves observed simultaneously at the dawn and dusk flanks of the Earth’s magnetopause","authors":"Niklas Grimmich ,&nbsp;Adriana Settino ,&nbsp;Heidi Katariina Nykyri ,&nbsp;Martin Owain Archer ,&nbsp;Kevin-Alexander Blasl ,&nbsp;Adrian Pöppelwerth ,&nbsp;Rumi Nakamura ,&nbsp;Ferdinand Plaschke","doi":"10.1016/j.pss.2025.106182","DOIUrl":"10.1016/j.pss.2025.106182","url":null,"abstract":"<div><div>Across the Earth’s magnetopause, unless the magnetic fields stabilise the boundary, the velocity shear between the magnetospheric plasma and the shocked plasma of the solar wind can lead to the Kelvin–Helmholtz instability. This instability can develop into large-scale surface waves and vortices at the magnetopause, causing the different plasma regions to mix, which plays an important role in the transfer of energy across the magnetopause. We know from spacecraft observations and simulations that the way Kelvin–Helmholtz waves grow and evolve can be different at dawn and dusk. However, very few studies have directly observed this phenomenon on both flanks of the magnetopause simultaneously, nor have they provided a consistent explanation for the question of symmetrical or asymmetrical dawn–dusk growth of the waves. By combining measurements from the THEMIS and Cluster missions, we can report here on an event where such a simultaneous observation of the Kelvin–Helmholtz waves is possible.</div><div>For this event, we investigate and compare the typical wave parameters and the plasma mixing on the two flanks. Our results suggest an asymmetric evolution of the Kelvin–Helmholtz waves at dawn and dusk. Comparing these results with previous studies of simultaneously observed events and linking them to solar wind conditions further shows that this asymmetric growth seems to occur during the Parker spiral IMF, but probably only if the magnetic fields are strong enough to effectively stabilise the boundary at the dusk flank due to field line draping.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"267 ","pages":"Article 106182"},"PeriodicalIF":1.7,"publicationDate":"2025-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144867090","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 generic compensation method for dynamic systematic errors in the geolocation of linear pushbroom satellite imagery","authors":"Da Li ,&nbsp;Yonghua Jiang ,&nbsp;Jingyin Wang ,&nbsp;Shaodong Wei ,&nbsp;Guo Zhang ,&nbsp;Huilong Wang","doi":"10.1016/j.pss.2025.106139","DOIUrl":"10.1016/j.pss.2025.106139","url":null,"abstract":"<div><div>In Earth observation and planetary exploration missions, high-precision geolocation through remote sensing is crucial. However, dynamic systematic errors in satellite imagery and ancillary flight data, arising from sensor limitation and measurement technology, challenge traditional correction methods such as orientation image model and bias compensation model. This study proposes a piecewise bias matrix compensation method to improve the geolocation accuracy of linear pushbroom cameras by effectively eliminating dynamic systematic errors. The method focuses on detect orientation point exposure time utilizing the distribution characteristics of the reprojection residuals caused by dynamic system errors. This is accomplished through a stepwise strategy involving residual point cloud thinning and iterative end-point fitting algorithms, which automatically divide the sub-compensation model. Furthermore, considering the stability of the satellite’s flight attitude, a Lagrange interpolation method is introduced in the piecewise bias matrix compensation model, enhancing the internal consistency and absolute accuracy in the geometric positioning process of the optical linear pushbroom satellite. A comparison of the initial camera positioning results in the experimental dataset revealed that the reprojected errors of conjugate points in the MEX-HRSC can now achieve sub-pixel accuracy, with a maximum root mean square error of 0.54 pixels; the reprojected errors of GCPs in the XX-18 can now achieve sub-pixel accuracy, with a maximum root mean square error of 0.80 pixels. Additionally, building upon the elimination of dynamic systematic errors, this study constructs high spatial resolution DTMs of the Martian surface using high-resolution stereo imagery from the MEX-HRSC. These techniques and methods result in the intersection of corresponding rays in stereo pairs, which is crucial for subsequent 3D reconstruction.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"267 ","pages":"Article 106139"},"PeriodicalIF":1.7,"publicationDate":"2025-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144842496","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":"Directional Analysis of Fractures at ESA’s Rosalind Franklin landing site, Oxia Planum, Mars","authors":"Andrea Apuzzo ,&nbsp;Alessandro Frigeri ,&nbsp;Francesco Salvini ,&nbsp;Jeremy Brossier ,&nbsp;Maria Cristina De Sanctis ,&nbsp;Francesca Altieri ,&nbsp;Gene Walter Schmidt ,&nbsp;Ma_MISS team","doi":"10.1016/j.pss.2025.106169","DOIUrl":"10.1016/j.pss.2025.106169","url":null,"abstract":"<div><div>The Rosalind Franklin rover of the European Space Agency’s ExoMars program is going to land at Oxia Planum, Mars after its launch scheduled in 2030. The mission aims to look for evidence of past and present life on Mars. The presence of fractured rocks at the landing site is of interest to the astrobiological goal of the mission because fractures represent conduits that could facility circulation of fluids. Our study is devoted to observing the orientations of the fractures and to investigate their possible origin by single or multiple processes. We first selected 50 regions of interest (ROIs) in areas of pronounced fracturing, using images from the High-Resolution Imaging Science Experiment (HiRISE) as a basemap. We then analysed the orientation of the fractures and how it varied with length. Statistical analysis shows that fractures predominantly have an E-W orientation, especially in longer fractures, while shorter fractures have a more random pattern. These orientation trends suggest a geological history influenced primarily by both hydrofracturing and tectonic processes. The preferred orientation, which is consistent with north-south tectonic shortening structures documented in the vicinity of the region, is likely to reflect a regional tectonic event between 3.7 and 4.0 billion years ago. The origin of the fractures may have promoted the migration of subsurface fluids through the fractured bedrock, potentially creating habitable conditions for microbial life. Our first study on fractures supports other studies on the geology of the ancient terrains at Oxia Planum, which hides a complex geologic history needing to be unravelled from different perspectives.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"267 ","pages":"Article 106169"},"PeriodicalIF":1.7,"publicationDate":"2025-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144907006","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":"Comet 12P/Pons-Brooks: Dust properties","authors":"R.S. Garcia ,&nbsp;E. Fernández-Lajús ,&nbsp;R.P. Di Sisto ,&nbsp;R.A. Gil-Hutton","doi":"10.1016/j.pss.2025.106181","DOIUrl":"10.1016/j.pss.2025.106181","url":null,"abstract":"<div><div>Comet 12P/Pons-Brooks, a Halley-type comet with a 71-year orbital period, was first discovered in 1812. It follows a highly inclined trajectory, originating from just beyond Neptune’s orbit. Ground-based observations have shown that the comet exhibited activity at a heliocentric distance of 11 au during its approach to the Sun. Numerous studies have since focused on its behavior, particularly its pre-perihelion outbursts, which have provided valuable insights into its dynamic and volatile nature.</div><div>This study examines the dust behavior of 12P following its perihelion passage. Using the 0.6 m Helen Sawyer Hogg telescope at the Complejo Astronómico El Leoncito (CASLEO), a series of images were captured between May and June 2024 using broadband I, R, and V filters. Morphological, photometric, and numerical analyses were performed to investigate the comet’s dust characteristics. Enhanced imaging revealed two active regions within an isotropic coma, which contributed to its distinctive “devil comet” appearance. Photometric analysis, based on the magnitudes and dust production rate from the <span><math><mrow><mi>A</mi><mrow><mo>(</mo><mn>0</mn><mo>°</mo><mo>)</mo></mrow><mi>f</mi><mi>ρ</mi></mrow></math></span> parameter, indicated ordinary dust behavior, with no characteristic outbursts observed.</div><div>To gain further insights into 12P’s dust behavior, the data were fitted to a new theoretical model for studying dust in comets. This model suggests that the dust coma primarily consisted of large particles emitted from two high-latitude active areas at a velocity of approximately <span><math><mrow><mn>409</mn><mspace></mspace><msup><mrow><mtext>ms</mtext></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></mrow></math></span>, assuming a rotation period of 57 h.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"267 ","pages":"Article 106181"},"PeriodicalIF":1.7,"publicationDate":"2025-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144867091","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}