Planetary and Space Science最新文献

{"title":"In-mission synergy of science and navigation ephemeris products—Potential benefits for JUICE statistical Delta-V expenditure and beyond","authors":"J. Hener,&nbsp;S. Fayolle,&nbsp;D. Dirkx","doi":"10.1016/j.pss.2024.106017","DOIUrl":"10.1016/j.pss.2024.106017","url":null,"abstract":"<div><div>In 2031 the JUICE spacecraft will perform a multi-flyby tour of the Jovian system. Next to the radiometric tracking that is performed for navigation operations, the dedicated radio science instrument (3GM) collects high-accuracy radiometric measurements during the flybys.</div><div>We investigate the capability of the radio science data to provide improved moon state knowledge during navigational operations. We introduce ephemeris updates from radio science data into our simulated navigation operations and examine the potential savings of statistical <span><math><mrow><mi>Δ</mi><mi>V</mi></mrow></math></span> for corrective manoeuvres. A navigation orbit determination (OD) solution was simulated for the multi-flyby tour of JUICE, including the resulting state knowledge evolution of the Galilean moons. The OD was extended by an interface for external moon ephemeris updates, which was used to evaluate the impact of radio science generated external ephemerides on the statistical <span><math><mrow><mi>Δ</mi><mi>V</mi></mrow></math></span> budgets for post-flyby cleanup manoeuvres.</div><div>The moon state knowledge evolution during navigation operation showed a rapid reduction of the a-priori moon state uncertainty, for which the navigational tracking data coverage of the long, early tour arcs was identified as the driving factor. As a result of the longer tracking arcs, the moon state knowledge from navigation data results improves more quickly during the initial phase of the tour. Since the impact of moon state knowledge on the corrective manoeuvres is largest in this initial phase, the comparative analysis of the statistical <span><math><mrow><mi>Δ</mi><mi>V</mi></mrow></math></span> cost shows that the adoption of radio science ephemeris products does not effectuate significant <span><math><mrow><mi>Δ</mi><mi>V</mi></mrow></math></span> savings. Instead we showed that in order to achieve substantial <span><math><mrow><mi>Δ</mi><mi>V</mi></mrow></math></span> savings improvements of Europa’s and Ganymede’s ephemerides are required ahead of JUICE’s arrival.</div><div>While the analysis concludes that data synergies are unlikely to benefit the navigational operations, it highlights other potential synergies between the navigation and radio science data. A comparatively strong signature of Io’s dynamics was found in the simulated navigation data along the long early tour arcs, which could be leveraged for the benefit of the new global moon ephemeris solutions after JUICE.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"255 ","pages":"Article 106017"},"PeriodicalIF":1.8,"publicationDate":"2025-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143177379","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":"The effectiveness of microwave heating as an ISRU extraction technique on different arrangements of icy lunar regolith","authors":"James D. Cole ,&nbsp;Simon Sheridan ,&nbsp;Sungwoo Lim ,&nbsp;Hannah M. Sargeant ,&nbsp;Mahesh Anand ,&nbsp;Hannah Chinnery ,&nbsp;James Mortimer ,&nbsp;Andrew Morse","doi":"10.1016/j.pss.2024.106011","DOIUrl":"10.1016/j.pss.2024.106011","url":null,"abstract":"<div><div>The lunar poles potentially contain vast quantities of water ice. The water ice is of interest due to its capability to answer scientific questions regarding the Solar System's water reservoir and its potential as a useable space resource for the creation of a sustainable cislunar economy. The lunar polar water ice exists in extremely harsh conditions under vacuum at temperatures as low as 40 K. Therefore, finding the most effective technique for extracting this water ice is an important aspect of ascertaining the suitability of lunar water as an economically viable space resource. Based on previous work, this study investigates the impact of the different possible arrangements of icy regolith in the lunar polar environment on the suitability of microwave heating as a water extraction technique. Three arrangements of icy regolith analogues were created: permafrost, fine granular, and coarse granular. The samples were created to a mass of 40 g, using the lunar highlands simulant LHS-1, and a target water content of 5 wt %. The samples were processed in a microwave heating unit using 250 W, 2.45 GHz microwave energy for 60 min. The quantity of water extracted was determined by measuring the sample mass change in real-time during microwave heating and the sample mass before and after heating. The permafrost, fine granular, and coarse granular samples had extraction ratios of 92 %, 83 %, and 97 %, respectively. Possible explanations for the observed variations seen in the mass loss profiles of the respective samples are provided, including explanations for the differences between samples of varying ice morphology (permafrost and granular) and the differences between samples with varying ice surface areas (fine and coarse granular). While differences were observed, microwave heating effectively extracted water in all the samples and remains an effective ISRU technique for extracting water from icy lunar regolith. Differences in the water extraction of different icy regolith could be useful in determining the arrangement of ice in buried samples.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"255 ","pages":"Article 106011"},"PeriodicalIF":1.8,"publicationDate":"2025-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143177380","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":"Microbial abundance across a salinity and mineralogical transect in the Ntwetwe Pan of Botswana: A terrestrial analogue for playa deposits on Mars","authors":"Fulvio Franchi ,&nbsp;Cassaro A ,&nbsp;Cavalazzi B ,&nbsp;Lebogang L ,&nbsp;Tarozzi A ,&nbsp;Kahsay T. H ,&nbsp;Pacelli C","doi":"10.1016/j.pss.2024.106028","DOIUrl":"10.1016/j.pss.2024.106028","url":null,"abstract":"<div><div>The current conditions of the Martian surface are considered prohibitive for life as we know it, due to strong radiation, highly oxidizing conditions, concentrated evaporative salts (including highly toxic perchlorates), and relatively low water activity. Earth hosts a multitude of extreme environments whose physico-chemical properties partly match Martian conditions. Such environments are defined as “analogue sites” and may offer a critical test-bed for astrobiological studies in characterizing the physical and chemical boundaries within which terrestrial life may exist and in assessing the habitability of Mars, and understanding the biological mechanisms for survival in extreme environments.</div><div>For example, the Makgadikgadi Basin, located in central Botswana is considered one of the largest evaporitic basins on Earth, characterized by deposition of NaCl crusts from brines and surface water, high UV radiation and strong evaporitic conditions. These conditions may be compared with those detected on the Martian surface and/or hypothesized for early Mars.</div><div>Here, we provide, for the first time, a comparison between the abundance of microorganisms (both bacteria and fungi) and the chemical and physical properties of the surficial sediments from the Ntwetwe Pan, in the western Makgadikgadi Basin, providing a description of the morphological characteristics of halophilic communities and highlighting interactions with different mineral phases. These results show that fungi communities are more prone to variations due to changes in salinity and evaporite mineralogy. In general, the abundant filaments found in the surface sediments of the Makgadikgadi pans provide templating for the nucleation of carbonates and other evaporitic minerals such as trona and thenardite.</div><div>This study draws links between the effects of a hypersaline environment on the survival potential (abundance) of microorganisms and their preservation potential within mineral phases. Studies of the Makgadikgadi pans could help to understand if hypothetical life-forms may exist or have existed on Mars, and if they are likely to be preserved in the evaporitic playa deposits described across the planet.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"255 ","pages":"Article 106028"},"PeriodicalIF":1.8,"publicationDate":"2025-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143176540","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":"Kinetic theory for rings around oblate central bodies","authors":"Shribharath B.","doi":"10.1016/j.pss.2024.106033","DOIUrl":"10.1016/j.pss.2024.106033","url":null,"abstract":"<div><div>We apply kinetic theory (KT) to solve for the vertical structure of an axisymmetric, self-gravitating, particulate ring around a spheroidal central body which may be either spherical or oblate. Our work improves upon the present KT models of rings by introducing a more general central body potential. We consider both dilute and dense rings. As an example for a dilute ring, we solve for the vertical structure of Saturn’s A ring including Saturn’s oblateness in our calculations. We compare our results with earlier works (Simon and Jenkins 1994) which assumed a spherical Saturn. Then, we calculate the corrections due to the oblateness on the ring stability condition obtained by them. We find that the planetary oblateness adversely affects ring stability due to the enhanced shearing. Next, we add self-gravity as an additional vertical force in dilute rings, where particle clumping is negligible, and find the combined stability boundary. Self-gravity is seen to have a stabilising effect on the ring as reported in earlier studies (Salo 1995), though, its stabilising effect is observed to be less than the destabilising effect of the oblateness of the central body, at least, for dilute rings. Then, we move to moderately dense rings. Oblateness of the central body is seen to perturb the ring properties, and, the results indicate a good qualitative comparison with DE simulations of Gupta et al., (2018). However, we note the emergence of strong self-gravity wakes in dense rings, an aspect that is usually ignored in kinetic theory for rings. Hence, we show the need for improved constitutive modelling of rings including the mesoscopic inhomogeneities in the form self-gravity wakes. Finally, we apply KT to solve for the vertical structure of Chariklo’s inner ring. Through this we estimate the 1/3 resonance torque of Chariklo that acts on the inner boundary of Chariklo’s inner ring by calculating the shear stress in the ring. Overall, our work demonstrates the structural differences of rings around minor planets like Chariklo that have highly oblate shapes.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"255 ","pages":"Article 106033"},"PeriodicalIF":1.8,"publicationDate":"2025-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143176541","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":"Enhancing discrete element model accuracy for lunar soil: Calibration and validation of mesoscopic parameters","authors":"Xianghui Bu ,&nbsp;Yuqiong Li ,&nbsp;Na Li ,&nbsp;Liping Ying ,&nbsp;Zheng Yuan ,&nbsp;Zongfang Han ,&nbsp;Xiuli Xu","doi":"10.1016/j.pss.2024.106024","DOIUrl":"10.1016/j.pss.2024.106024","url":null,"abstract":"<div><div>To enhance the precision of the discrete element model for lunar soil-tool simulation work, this paper introduces a novel discrete element model of lunar soil incorporating particle shape and the van der Waals forces between particles. The effect of mesoscopic parameters on peak stress and failure point are systematically calibrated in the model by triaxial compression stress-strain curves. The results show that six <em>meso</em>-parameters have significant impact on the mechanical response of the model, including effective modulus, rolling friction coefficient, normal-to-shear stiffness ratio, damping coefficient, maximum attractive force and attraction range. The model accurately simulates complex mechanical behavior in both loose, dense lunar soils and soil-tool interaction. This study lays a foundation for future lunar soil-anchor interaction simulation and the interpretation of lunar soil mechanical parameters.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"255 ","pages":"Article 106024"},"PeriodicalIF":1.8,"publicationDate":"2025-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143177381","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":"Chemical changes in terrestrial lunar simulants exposed to gamma radiation simulating lunar ionizing radiation environment","authors":"Nilanjan Mitra ,&nbsp;Tyrel M. McQueen ,&nbsp;Robert Volpe ,&nbsp;Michael Daly ,&nbsp;V. Desai ,&nbsp;N.P. Armitage","doi":"10.1016/j.pss.2024.106031","DOIUrl":"10.1016/j.pss.2024.106031","url":null,"abstract":"<div><div>Recent research has focused on using in-situ lunar materials for infrastructural construction to develop sustainable lunar infrastructure for human habitats. The development of any infrastructural material for construction typically involves some chemical reactions. For lunar infrastructural construction research, terrestrially derived lunar simulants (which match the chemical compositions and particle size of actual lunar samples from the Apollo and Luna missions) are typically utilized for these feasibility studies. However, there are differences between these lunar simulants and the actual lunar regolith, since the simulants are not subjected to ionizing radiations from galactic cosmic radiation (GCR) and solar energetic particles (SEP) prevalent on the moon. In this study, the simulant materials were subjected to gamma radiation to simulate similar ionizing conditions on Earth. It is demonstrated in this manuscript that gamma irradiation results in the formation of entrapped radicals, which significantly changes the chemical signatures of the terrestrially derived lunar simulants (characterized using Terahertz and Electron Paramagnetic resonance spectroscopy), raising questions and describing the need for further detailed material investigations for the terrestrial methodologies being developed for in-situ resource utilization (ISRU) for lunar construction.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"255 ","pages":"Article 106031"},"PeriodicalIF":1.8,"publicationDate":"2025-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143176543","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":"Characterizing heterogeneities in the subsurface with an ultra-wideband GPR: Application to WISDOM, the GPR of the Rosalind Franklin ExoMars mission","authors":"E. Brighi ,&nbsp;V. Ciarletti ,&nbsp;A. Le Gall ,&nbsp;D. Plettemeier ,&nbsp;Y. Hervé ,&nbsp;N. Oudart ,&nbsp;C. Quantin-Nataf ,&nbsp;M. Gilles ,&nbsp;F.-W. de Lamberterie","doi":"10.1016/j.pss.2024.106012","DOIUrl":"10.1016/j.pss.2024.106012","url":null,"abstract":"<div><div>Ultra-wideband Ground Penetrating Radars (GPR) are sensitive to a large range of scatterer sizes. Considering fractal heterogeneities in the subsurface, we propose a method to retrieve their typical size <em>L</em>. The determination of <em>L</em> with this method does not require <em>a priori</em> knowledge of the statistical distribution of permittivity values in the investigated subsurface. The method relies on the analysis of the backscattered signal by frequency/wavelength sub-bands. It is adapted to WISDOM, the GPR onboard the rover of the Rosalind Franklin ExoMars mission (ESA), but can be applied to any ultra-wideband GPR. Based on numerical simulations, a maximum in volume backscattering is reached at the wavelength (in the subsurface) <span><math><mrow><mi>λ</mi><mo>=</mo><mrow><mo>(</mo><mrow><mn>5.3</mn><mo>±</mo><mn>0.2</mn></mrow><mo>)</mo></mrow><mi>L</mi></mrow></math></span>. We demonstrate that this maximum, and therefore <em>L</em>, can be identified even in presence of moderate electrical losses, compatible with conditions expected on the Moon or Mars. Assuming an average permittivity of 5, WISDOM (0.5–3 GHz) data products could be used to estimate <em>L</em> as long as it is in the range 0.9–4.2 cm. The retrieval method for <em>L</em> is validated on experimental WISDOM data acquired in a controlled environment.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"255 ","pages":"Article 106012"},"PeriodicalIF":1.8,"publicationDate":"2025-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143177382","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 mapping and characterization of the NW-Phoebe volcano-magmatic center on Venus","authors":"E.G. Antropova ,&nbsp;C.H.G. Braga ,&nbsp;R.E. Ernst ,&nbsp;H. El Bilali ,&nbsp;J.W. Head ,&nbsp;K.L. Buchan ,&nbsp;A. Shimolina","doi":"10.1016/j.pss.2024.105996","DOIUrl":"10.1016/j.pss.2024.105996","url":null,"abstract":"<div><div>Detailed geological mapping (at 1:500,000 scale) of the area located in the eastern part of the BAT region, northwest of Phoebe Regio (∼4°N to 1°S; ∼85° to 78°W) using Magellan SAR images has distinguished 48 volcano-tectonic units and 22 structural units. Stratigraphically, the oldest units are represented by fragments of the tesserae, densely lineated plains and other plains units. Younger units include lobate flow fields oriented in various directions (NE, E, SW) and flows associated with shield clusters.</div><div>The post-tesserae evolutionary model proposed for this region distinguishes two Stages, early (I) and late (II), and explains the sequence of formation of all the geological features in terms of intraplate magmatism. Stage I consists of multiple corona structures and associated volcanism that are widely dispersed over the study area. Stage II consists of an intermediate-scale volcano with multiple lava flows radiating approximately from its center, and a field of small shield volcanoes near the summit. The units of Stage II appear to be approximately coeval and to define a distinct volcanic event covering an areal extent of ⁓250,000 km², that we have termed the NW-Phoebe event.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"254 ","pages":"Article 105996"},"PeriodicalIF":1.8,"publicationDate":"2024-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142746080","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":"Modeling the interstellar dust detections by DESTINY+ I: Instrumental constraints and detectability of organic compounds","authors":"Harald Krüger ,&nbsp;Peter Strub ,&nbsp;Maximilian Sommer ,&nbsp;Georg Moragas-Klostermeyer ,&nbsp;Veerle J. Sterken ,&nbsp;Nozair Khawaja ,&nbsp;Mario Trieloff ,&nbsp;Hiroshi Kimura ,&nbsp;Takayuki Hirai ,&nbsp;Masanori Kobayashi ,&nbsp;Tomoko Arai ,&nbsp;Jon Hillier ,&nbsp;Jonas Simolka ,&nbsp;Ralf Srama","doi":"10.1016/j.pss.2024.106010","DOIUrl":"10.1016/j.pss.2024.106010","url":null,"abstract":"<div><div>The DESTINY<span><math><msup><mrow></mrow><mrow><mo>+</mo></mrow></msup></math></span> spacecraft will be launched to the active asteroid (3200) Phaethon in 2025. The spacecraft will be equipped with the DESTINY<span><math><msup><mrow></mrow><mrow><mo>+</mo></mrow></msup></math></span> Dust Analyzer (DDA) which will be a time-of-flight impact ionization mass spectrometer. In addition to the composition of impacting dust particles, the instrument will measure the particle mass, velocity vector, and surface charge. Here, we study the detection conditions of DDA for interstellar dust during the DESTINY<span><math><msup><mrow></mrow><mrow><mo>+</mo></mrow></msup></math></span> mission. We use the interstellar dust module of the Interplanetary Meteoroid environment for EXploration model (IMEX Sterken et al., 2013; Strub et al., 2019) to simulate the flow of interstellar dust through the Solar System. Extending earlier work by Krüger et al. (2019b) we consider the entire DESTINY<span><math><msup><mrow></mrow><mrow><mo>+</mo></mrow></msup></math></span> mission, i.e. the Earth-orbiting phase of the spacecraft during the initial approximately 1.5 years after launch, the nominal interplanetary mission phase up to the Phaethon flyby, and a four-years mission extension beyond the Phaethon flyby. The latter may include additional asteroid flybys. For predicting dust fluxes and fluences we take into account a technical constraint for DDA not to point closer than <span><math><mrow><mn>90</mn><mo>°</mo></mrow></math></span> towards the Sun direction for health and safety reasons of the instrument and in order to avoid electrical noise generated by photoelectrons. For the Earth orbiting phase after launch of DESTINY<span><math><msup><mrow></mrow><mrow><mo>+</mo></mrow></msup></math></span> our simulations predict that up to 28 interstellar particles will be detectable with DDA in 2026. In the following years the interplanetary magnetic field changes to a focussing configuration for small (<span><math><mrow><mo>≲</mo><mn>0</mn><mo>.</mo><mn>1</mn><mspace></mspace><mi>μ</mi><mi>m</mi></mrow></math></span>) interstellar dust particles. This increases the total number of detectable particles to 50 during the interplanetary mission of DESTINY<span><math><msup><mrow></mrow><mrow><mo>+</mo></mrow></msup></math></span> in 2027. In 2028 and 2029/30 approximately 160 and 190 particles will be detectable, respectively, followed by about 500 in 2030/31. We also make predictions for the detectability of organic compounds contained in the interstellar particles which is a strong function of the particle impact speed onto the detector. While organic compounds will be measurable only in a negligible number of particles during the Earth orbiting and the nominal interplanetary mission phases, a few 10s of interstellar particle detections with measurable organic compounds are predicted for the extended mission from 2028 to 2031.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"254 ","pages":"Article 106010"},"PeriodicalIF":1.8,"publicationDate":"2024-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142746082","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":"Induced polarization in the transient electromagnetic method for detection of subsurface ice on Earth, Mars, and the Moon","authors":"Erlend Finden ,&nbsp;Roar Skartlien ,&nbsp;Sverre Holm ,&nbsp;Svein-Erik Hamran","doi":"10.1016/j.pss.2024.106007","DOIUrl":"10.1016/j.pss.2024.106007","url":null,"abstract":"<div><div>The transient electromagnetic method (TEM) can capture an induced polarization (IP) signature of subsurface ice. Using numerical modeling of a horizontally layered earth, we investigate how IP in TEM can be exploited for subsurface ice detection on Earth, Mars, and the Moon. In the model we implement electrical parameters from laboratory measurements of ice, planetary regolith simulants, and terrestrial soil from the literature. In contrast to currently applied forward models, we include two Cole–Cole relaxation terms to model the dielectric relaxation of adsorbed water or salt hydrate in addition to the relaxation of ice. On Earth, IP signals of shallow layers of silt mixed with 44–100 vol% ice embedded in resistive host layers of 3 k<span><math><mi>Ω</mi></math></span>m can be detected. Both at mid (45<span><math><msup><mrow></mrow><mrow><mo>∘</mo></mrow></msup></math></span> N) and lower (35<span><math><msup><mrow></mrow><mrow><mo>∘</mo></mrow></msup></math></span> N) latitudes on Mars, meter thick layers of massive ice can be detected at 10 m depth if the ice contains salts. Corresponding layers of 60 vol% ice mixed with Martian regolith simulant show similar detectability. For IP signals of lunar ice to be detected in ice volume fractions of 7.4%–46%, a development in TEM technology is required, including mitigation of early time interference, or enhancing the signal to noise level.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"254 ","pages":"Article 106007"},"PeriodicalIF":1.8,"publicationDate":"2024-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142746081","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}