Planetary and Space Science最新文献

{"title":"Optimal choice of closest approach distance for a comet flyby: Application to the Comet Interceptor mission","authors":"J. De Keyser ,&nbsp;N.J.T. Edberg ,&nbsp;P. Henri ,&nbsp;H. Rothkaehl ,&nbsp;V. Della Corte ,&nbsp;M. Rubin ,&nbsp;R. Funase ,&nbsp;S. Kasahara ,&nbsp;C. Snodgrass","doi":"10.1016/j.pss.2024.106032","DOIUrl":"10.1016/j.pss.2024.106032","url":null,"abstract":"<div><div>A comet flyby, like the one planned for the Comet Interceptor mission, takes place under conditions that remain largely unknown up to the moment of encounter. A detailed trajectory design phase, which includes verification of the technical limitations implied by the flyby geometry, precedes target comet selection. Thus the flyby velocity and the solar zenith angle at closest approach are known in advance. Solar irradiance and the neutral gas expansion speed can be estimated reasonably well. However, the comet outgassing rate, the dust production rate, and the solar wind conditions are only known within broader uncertainty margins. The present paper aims to optimally choose the one degree of freedom that is available for tuning the flyby conditions: the distance of closest approach. This choice is based on a simplified formalism that expresses, on one hand, the science return to be expected as a function of the closest approach distance, and, on the other hand, the risks implied by a close approach. This is done by performing Monte Carlo simulations over a large sample of possible comet flyby configurations, based on the expected probability distributions of the gas and dust production rates and the solar wind conditions, for different closest approach distances. For small flyby distances, a spacecraft has the opportunity to study the nucleus, the neutral gas coma, and the induced magnetosphere from up close, benefiting the science return. There is a trade-off to be made against the cometary dust collision risk, which becomes larger close to the nucleus. This trade-off is illustrated for the case of the Comet Interceptor main spacecraft and the two probes it plans to release. The change of the optimal flyby distance with gas and dust production rate, solar EUV flux, and flyby speed is discussed.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"256 ","pages":"Article 106032"},"PeriodicalIF":1.8,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143262389","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"High resolution olivine abundance mapping in the Copernicus crater combining spectral data of Chandrayaan-1 M3 and Kaguya MI","authors":"Yehor Surkov ,&nbsp;Urs Mall ,&nbsp;Viktor Korokhin","doi":"10.1016/j.pss.2025.106039","DOIUrl":"10.1016/j.pss.2025.106039","url":null,"abstract":"<div><div>We present a technique for improving the spatial resolution of satellite spectrophotometric data of the Moon's surface using an artificial neural network. We demonstrate this approach using the high-spectral low-spatial resolution Moon Mineralogy Mapper (M³) spectrophotometer and the low-spectral high-spatial resolution Multiband Imager (MI) Kaguya datasets for super-resolution olivine mapping over the Copernicus crater. The super-resolution of spectral maps is achieved by correlating spectral data of these instruments using a multilayer perceptron. An important advantage of the method is the use of a single data frame from each dataset to study a particular lunar region. The obtained maps of the olivine abundance provide new spatial context of the investigated mineral distribution: olivine-rich surface units become visible primarily as flow tubes, lava ponds on the crater walls and boulder outcrops associated with high olivine content (up to 90 vol%) at the central peak of the investigated crater. The content of the olivine-reaches deposits of the area on the central peak reaches up to 35 vol % of the lunar regolith.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"256 ","pages":"Article 106039"},"PeriodicalIF":1.8,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143262394","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Compositional mapping and geological age of the mare basalts of the southern quadrangle of Moon","authors":"D. Paul ,&nbsp;S. Dhoundiyal ,&nbsp;A. Porwal ,&nbsp;G. Thangjam","doi":"10.1016/j.pss.2025.106034","DOIUrl":"10.1016/j.pss.2025.106034","url":null,"abstract":"<div><div>Spectral parameters of pyroxene estimated from the Moon Mineralogy Mapper (M³) hyperspectral data are used to delineate a total of twenty-two distinct compositional units in the southern quadrangle of the Moon (0°S to 30°S and 5°W to 30°W) covering four mare regions, namely, south-east Oceanus Procellarum, Mare Humorum, Mare Cognitum, and Mare Nubium. The compositional variation of pyroxenes and inferred crystallization temperatures indicate contrasting magmatic emplacement activity in the studied area. This finding is further strengthened by examining the variations in the FeO and TiO₂ content where units with titanium content (&gt;5.9 wt%) are associated with calcium content (&gt;30 wt%). The study further reveals two possible sources of magma, namely, a high titanium (Ti) high calcium pyroxene (HCP) magma source and a moderately titanium-rich high calcium pyroxene (HCP) magma source. Our crater size-frequency distribution (CSFD) study indicates that the volcanism prevailed in the study area from approximately 3.6 Ga to 0.73 Ga, peaking around ∼2.9 Ga to 1.5 Ga.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"256 ","pages":"Article 106034"},"PeriodicalIF":1.8,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143262390","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":"Potential bedrock exposures of Schrödinger impact melt sheet and/or polymict impact breccias within a crater floor fracture system and volcanic vent","authors":"David A. Kring ,&nbsp;Valentin T. Bickel ,&nbsp;Pascal Lee ,&nbsp;Amy L. Fagan ,&nbsp;Jennifer L. Heldmann ,&nbsp;Rick C. Elphic ,&nbsp;David J. Lawrence ,&nbsp;Timothy J. Parker ,&nbsp;Harrison H. Schmitt","doi":"10.1016/j.pss.2025.106063","DOIUrl":"10.1016/j.pss.2025.106063","url":null,"abstract":"<div><div>The Schrödinger impact basin provides significant geological targets for future exploration, including impact melts, multi-kilometer-long exposures of magmatic rocks from deep within the lunar crust, volcanic mare, pyroclastic ash deposits, potentially with mantle xenoliths, and a geophysical setting for examining the near-rim structure of the South Pole-Aitken mega-basin. Surveyor, Ranger, and Apollo programs confirmed that constant gardening of the lunar surface by impact cratering processes reduces the availability of outcrops, which are those key bedrock exposures that geologists on Earth use as the most reliable sources of information about planetary evolution. Lunar Reconnaissance Orbiter Camera (LROC) images of the lunar surface are providing data needed to identify bedrock exposures on the Moon, and tracked boulders leading to rock exposures, in locations suitable for future exploration. One such rocky exposure occurs within a volcanic vent within the Schrödinger impact basin. We consider six working hypotheses for its origin and conclude it likely represents a bedrock exposure of impact melt and/or impact breccia produced by the Schrödinger impact event or, alternatively, pristine lava rock associated with the vent's pyroclastic origin. While elsewhere in the basin those units are covered with regolith and younger volcanic deposits, the opening of a crater floor fracture and pyroclastic eruption of volcanic material cleared a vertical exposure through the impact or eruptive lithologies, which remain accessible for exploration today.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"257 ","pages":"Article 106063"},"PeriodicalIF":1.8,"publicationDate":"2025-01-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143284617","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Geological history of Theia Mons, Beta Regio plume, Venus: Recognition of two main magmatic centers for flows, radiating dyke swarms and triple junction rifting","authors":"A.S. Shimolina ,&nbsp;R.E. Ernst ,&nbsp;H. El Bilali ,&nbsp;D.G. Malyshev ,&nbsp;V.E. Rozhin ,&nbsp;E.G. Antropova","doi":"10.1016/j.pss.2025.106050","DOIUrl":"10.1016/j.pss.2025.106050","url":null,"abstract":"<div><div>Theia Mons (centered at 23.4° N, 79.4° W) is the main volcanic center for the Beta Regio plume, of the Beta-Atla-Themis (BAT) region, Venus. Synthetic aperture radar data (SAR) and altimetry data from the 1989–1994 NASA Magellan mission were used to produce a geological map and history of Theia Mons, revealing two distinct magmatic centers (200 km apart), each the focus of basaltic lava flows, extensional lineaments (representing the surface expression of dyke swarms), and associated rift zones. The study area spans 88°W to 72°W, 16°45′N to 29°45′N, and mapping was at 1:500,000 scale. Our detailed mapping makes this area a prime target for the future Venus missions (orbital and lander), also given that Beta Regio is a strong candidate for ongoing volcanic activity.</div><div>Lava (basaltic) flow units (88 distinguished on the basis of variation in radar backscatter) belonging to Theia Mons volcano were combined into 19 Flow Groups and then into 3 Flow Packages. The lava flows appear to diverge from two distinct magmatic centers, labelled Center 1 (24.5°N, 78.1°W) and Center 2 (23.4° N, 79.4°W), with the older Center 1 being obscured by the volcanism of the younger Center 2. Center 1 consists of flows with low radar brightness and which extend to a maximum to 830 km from the center. Center 2 coincides with the currently preserved central caldera and consists of lava flows of low radar brightness with a maximum length of 620 km, followed by a second pulse of radar-bright flows that are less extensive and concentrated near the center.</div><div>About 10,000 extensional lineaments (grabens, fissures, and fractures) were mapped and grouped into 19 systems, of which 15 are interpreted to overlie dyke swarms: 2 radiating systems are associated with Centers 1 and 2, and 13 other systems belong to other (older and likely unrelated) magmatic centers in the region. A partial circumferential swarm may also be present, associated with Center 2.</div><div>Four other extensional lineaments sets are inferred to represent sets of normal faults associated with rift zones (Devana and Zverine, and additional rift zones). These rift zones exhibit two sets of ‘triple junction’ geometry, which are approximately also focussed on the same Centers 1 and 2, revealed by the lava flows and rift zones.</div><div>An underlying mantle plume is interpreted to be responsible for the dykes, flows and triple junction rifting. The cause of the shift between Centers 1 and 2 (200 km to SW) is unknown, but plausible mechanisms include a shift of the lithospheric plate above a stationary single plume, or a bending of the mantle plume (e.g. in a mantle wind) between timing of Center 1 and Center 2 activity.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"257 ","pages":"Article 106050"},"PeriodicalIF":1.8,"publicationDate":"2025-01-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143284621","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Low temperature fluorescence excitation and emission spectra of molecules relevant to Mars: Chlorobenzene, benzoic acid, phthalic acid, mellitic acid, and benzene in water ice solutions at temperatures between 78 K and 273 K","authors":"Suresh Sunuwar,&nbsp;Carlos E. Manzanares","doi":"10.1016/j.pss.2025.106054","DOIUrl":"10.1016/j.pss.2025.106054","url":null,"abstract":"<div><div>The discovery of chlorobenzene detected in soil samples obtained in Mars has been the subject of several interpretations. The original sample was subjected to pyrolysis before the gas chromatography-mass spectrometry (GC-MS) separation and identification with the Sample Analysis at Mars (SAM) instrument on the Curiosity rover. It is believed that chlorobenzene detected at concentrations above the background level of the instrument was a product of other organic molecules reacting with perchlorates of the Martian soil. Mars surface temperatures may reach a high of about 293 K at noon, at the equator, and a low of about 120 K at the poles. In this paper, characteristic fluorescence excitation and emission spectra are presented for chlorobenzene and the suggested precursor molecules: benzoic acid, phthalic acid, and mellitic acid in transparent hexagonal water ice solutions at temperatures between 273 K and 78 K. In addition, the liquid solution spectra at 292 K. Spectra of benzene in water ice solutions have also been included. The experimental results presented in this paper are to be compared with fluorescence experiments of Mars missions that will explore the polar regions and other regions where water ice is expected to be found. Limits of detection at part per billion by mass (ng/g) concentrations at room temperature are discussed based on our results and the literature. The application of fluorescence for low temperature studies of Mars samples is also discussed with a proposed miniature instrument with a laser source to increase the sensitivity of the detection and could be used for solid or liquid samples.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"257 ","pages":"Article 106054"},"PeriodicalIF":1.8,"publicationDate":"2025-01-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143284560","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 Arctic analogue for the future exploration of possible biosignatures on Enceladus","authors":"F. Franchi ,&nbsp;M. Túri ,&nbsp;G. Lakatos ,&nbsp;K.K. Rahul ,&nbsp;D.V. Mifsud ,&nbsp;G. Panieri ,&nbsp;R. Rácz ,&nbsp;S.T.S. Kovács ,&nbsp;E. Furu ,&nbsp;R. Huszánk ,&nbsp;R.W. McCullough ,&nbsp;Z. Juhász","doi":"10.1016/j.pss.2025.106051","DOIUrl":"10.1016/j.pss.2025.106051","url":null,"abstract":"<div><div>Methane-rich emissions to the seafloor along the Arctic mid-oceanic ridge hold strong astrobiological significance, as they may represent analogues of putative hydrothermal vent environments on Enceladus. Although such environments on Enceladus would be ideal to sample in future astrobiological missions, this may not be possible due to technological and logistical limitations. As such, searching for biosignatures in the more readily sampled cryovolcanic plumes or Enceladus’ icy shell is preferable. In this regard, the Arctic Ocean, where the geologically active seafloor is covered by thousands of metres of salty water and sealed by an ice cap, is a unique terrestrial analogue of Enceladus. In the present study, we have sought to determine whether any geochemical biosignatures associated with methane cycling (e.g., elevated methane concentrations, carbon isotopic fractionation) can be detected in Arctic ice and seawater samples using mass spectrometric techniques similar to those likely to be included in the payloads of planned missions to Enceladus. Our results have shown that, although no unequivocal evidence of methane could be detected in our Arctic samples, the carbon isotopic composition of carbon dioxide gas and the oxygen isotopic composition of water vapour emitted from the Arctic samples could indeed be measured. Furthermore, an excess of molecular hydrogen with abundances comparable to the composition of Enceladus’ southern pole plume was possibly observed in one of the Arctic ice samples. These results have implications for detectable indirect geochemical evidence of putative ecosystems of hydrogenotrophic methanogenic life on the seafloor of Enceladus and justify future efforts at method development and refinement using apparatus similar to that likely to be included in the payloads of future missions.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"257 ","pages":"Article 106051"},"PeriodicalIF":1.8,"publicationDate":"2025-01-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143284622","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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":"Closed depressions on the surface of the Moon","authors":"Eulogio Pardo-Igúzquiza ,&nbsp;Peter Dowd","doi":"10.1016/j.pss.2025.106049","DOIUrl":"10.1016/j.pss.2025.106049","url":null,"abstract":"<div><div>This paper provides a new view of the lunar surface by using maps of its closed depressions which are not limited to impact craters. On the lunar landscape, in addition to impact craters of all sizes, there is a rich variety of other types of closed depressions related to impact, volcanism, tectonics and gravitational processes. Kilometre-scale closed depressions have been identified, delineated and mapped on the surface of the Moon by using the digital elevation model provided by the Lunar Orbiter Laser Altimeter (LOLA) instrument onboard the Lunar Reconnaissance Orbiter (LRO) spacecraft together with a pit filling algorithm. The map of closed depressions is a raster map of the same size and spatial resolution as the digital elevation model used to generate it and each pixel provides the depth with respect to the rim of the depression. A number of test sites were chosen to illustrate the methodology including impact basins, maria, highlands, volcanic terrain, intermediate terrain and modified terrain. These maps of closed depressions can be analysed in terms of their location, abundance, size, orientation, depth, geometry, asymmetry and irregularity together with other morphometric parameters. On average, 71% of the surface of the Moon is covered by closed depressions and that number decreases to around 55% for volcanic terrains. The histogram of the depths of the highlands test site can be considered as the standard depth histogram in which impact craters of all sizes cover the entire terrain. The histograms of the other zones vary from that standard profile. The ultimate purpose of this paper is to provide a tool for mapping closed-depressions on the lunar surface which may assist planetary geologists to identify geological processes and recognize geological formations in the study of the geology and geomorphology of the Moon.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"257 ","pages":"Article 106049"},"PeriodicalIF":1.8,"publicationDate":"2025-01-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143284559","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 dynamics of Atlas (S XV): Its current orbit and the recent past","authors":"Demétrio Tadeu Ceccatto ,&nbsp;Nelson Callegari Jr. ,&nbsp;Gabriel Teixeira Guimarães ,&nbsp;Karyna Gimenez","doi":"10.1016/j.pss.2024.106016","DOIUrl":"10.1016/j.pss.2024.106016","url":null,"abstract":"<div><div>This study comprehensively analyzes Atlas’s current orbit, focusing on the secular and resonant perturbations caused by Prometheus, Pandora, and Saturn’s oblateness. We performed numerical integration of the exact equations of motion for a dense ensemble of Atlas clone satellites. Through spectral analysis and interpretation of these orbits on dynamical maps, we identified the domain of the 54:53 Prometheus–Atlas and 70:67 Pandora–Atlas mean-motion resonances, showing that Atlas lies on the boundary of the separatrices of each of these resonances. We also identified the domains for the multiplets <span><math><msub><mrow><mi>Ψ</mi></mrow><mrow><mn>1</mn></mrow></msub></math></span>, <span><math><msub><mrow><mi>Ψ</mi></mrow><mrow><mn>2</mn></mrow></msub></math></span>, <span><math><msub><mrow><mi>Ψ</mi></mrow><mrow><mn>3</mn></mrow></msub></math></span> and <span><math><msub><mrow><mi>Ψ</mi></mrow><mrow><mn>4</mn></mrow></msub></math></span> associated with 70:67 resonance. Additionally, we explored the variation in Prometheus’s eccentricity, demonstrating that as eccentricity increases (or decreases) in the 54:53 resonance domain correspondingly decreases (or increases). This combined analysis, between the above mappings, revealed qualitatively the overlap between the 54:53 and 70:67 resonances, which are responsible for the chaotic behavior of Atlas’s orbit. We quantified chaotic motion in frequency space and found that the vicinity of Atlas is characterized by weak to moderate chaos, rather than strong chaos. Finally, we investigated Atlas’s recent past, considering Prometheus’s migration under the influence of Saturn’s tidal forces. This analysis reveals several resonances crossed in the past, particularly focusing on the Atlas–Prometheus pair, which exhibited a co-orbital configuration.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"255 ","pages":"Article 106016"},"PeriodicalIF":1.8,"publicationDate":"2025-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143176544","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":"Two methods for determining the temperature on the surface of the cometary nucleus based on spectroscopic measurements","authors":"Marcin Wesołowski ,&nbsp;Piotr Potera ,&nbsp;Krzysztof Kucab","doi":"10.1016/j.pss.2024.106027","DOIUrl":"10.1016/j.pss.2024.106027","url":null,"abstract":"<div><div>The paper presents two methods that can be used to determine the surface temperature of a cometary nucleus. The key role in this approach is played by the measurement of hemispherical albedo for selected dust analogues, which was performed using a Cary 5000 spectrometer. To most accurately reflect the actual structure of the dust layer present on the surface of the cometary nucleus under Earth’s conditions, selected dust analogues were used in laboratory research. In the first method, bolometric albedo (Bond albedo) was used, and in the second method, hemispherical albedo was used, which comes directly from the measurement. Comparing both methods, it was found that the average value of the temperature difference for a given analogue is 0.47 K. Due to the small temperature differences between these approaches, both methods can be treated as equivalent. Based on the measurements and calculations performed, it was found that the most representative analogue of the actual dust present on the surface of comet 67P/Churyumov–Gerasimenko is a sample consisting of a mixture of sand with a volume fraction of about 10% and charcoal with a volume fraction of about 90%.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"255 ","pages":"Article 106027"},"PeriodicalIF":1.8,"publicationDate":"2025-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143176546","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}