Pub Date : 2024-12-01DOI: 10.1016/j.pss.2024.105996
E.G. Antropova , C.H.G. Braga , R.E. Ernst , H. El Bilali , J.W. Head , K.L. Buchan , A. Shimolina
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.
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.
{"title":"Geological mapping and characterization of the NW-Phoebe volcano-magmatic center on Venus","authors":"E.G. Antropova , C.H.G. Braga , R.E. Ernst , H. El Bilali , J.W. Head , K.L. Buchan , 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 km<sup>2</sup>, 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}
Pub Date : 2024-12-01DOI: 10.1016/j.pss.2024.106010
Harald Krüger , Peter Strub , Maximilian Sommer , Georg Moragas-Klostermeyer , Veerle J. Sterken , Nozair Khawaja , Mario Trieloff , Hiroshi Kimura , Takayuki Hirai , Masanori Kobayashi , Tomoko Arai , Jon Hillier , Jonas Simolka , Ralf Srama
The DESTINY spacecraft will be launched to the active asteroid (3200) Phaethon in 2025. The spacecraft will be equipped with the DESTINY 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 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 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 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 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 () interstellar dust particles. This increases the total number of detectable particles to 50 during the interplanetary mission of DESTINY 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.
命运+宇宙飞船将于2025年发射到活动小行星（3200）法厄同。该航天器将配备命运+尘埃分析仪（DDA），这将是一个飞行时间撞击电离质谱仪。除了撞击尘埃颗粒的组成外，该仪器还将测量颗粒质量、速度矢量和表面电荷。在这里，我们研究了命运+任务期间DDA对星际尘埃的探测条件。我们使用星际尘埃模块的星际流星体环境探索模型(IMEX Sterken et al., 2013；Strub et al., 2019)来模拟星际尘埃在太阳系中的流动。扩展kr格尔等人（2019b）的早期工作，我们考虑整个DESTINY+任务，即在发射后大约1.5年的初始阶段，航天器的地球轨道阶段，名义的行星际任务阶段，直到法厄同飞越，以及法厄同飞越之后的四年任务扩展。后者可能包括额外的小行星飞越。为了预测尘埃通量和影响，我们考虑到DDA的技术限制，即为了仪器的健康和安全原因，不能指向太阳方向超过90°，并且为了避免光电子产生的电气噪声。在“命运+”发射后的地球轨道阶段，我们的模拟预测，到2026年，DDA将探测到多达28个星际粒子。在接下来的几年里，行星际磁场改变为一个聚焦小（小于0.1μm）星际尘埃粒子的结构。在2027年的“命运+”星际任务期间，这将使可探测粒子的总数增加到50个。在2028年和2029/30年，将分别检测到约160和190个颗粒，随后在2030/31年将检测到约500个颗粒。我们还预测了星际粒子中所含有机化合物的可探测性，这是粒子撞击探测器速度的一个强函数。虽然在地球轨道和名义的行星际任务阶段，有机化合物只能以可忽略不计的粒子数量进行测量，但预计在2028年至2031年的扩展任务期间，将有几十次星际粒子检测到可测量的有机化合物。
{"title":"Modeling the interstellar dust detections by DESTINY+ I: Instrumental constraints and detectability of organic compounds","authors":"Harald Krüger , Peter Strub , Maximilian Sommer , Georg Moragas-Klostermeyer , Veerle J. Sterken , Nozair Khawaja , Mario Trieloff , Hiroshi Kimura , Takayuki Hirai , Masanori Kobayashi , Tomoko Arai , Jon Hillier , Jonas Simolka , 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}
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 km can be detected. Both at mid (45 N) and lower (35 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.
{"title":"Induced polarization in the transient electromagnetic method for detection of subsurface ice on Earth, Mars, and the Moon","authors":"Erlend Finden , Roar Skartlien , Sverre Holm , 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}
Pub Date : 2024-12-01DOI: 10.1016/j.pss.2024.106015
Chenxu Zhao , Zongyu Yue , Kaichang Di , Yutong Jia , Wing-Huen Ip , Yangting Lin , Bo Wu , Biao Wang , Bin Xie
Previous studies have provided evidence for the synchronous rotation induced cratering asymmetry on lunar surface through numerical simulations and statistical analysis of a limited number of fresh craters. In this study, we reevaluated cratering asymmetry in lunar highland from (70°W, 60°N) to (70°E, 60°S) region using a new crater catalogue with diameters (D) ranging from 1 to 20 km. By utilizing a depth-to-diameter (d/D) ratio constraint to exclude the interference of degraded and secondary craters, we observed significant asymmetry in craters with d/D > 0.15. Moreover, leveraging the characteristic that larger diameter craters (D > 7 km) are less susceptible to degradation, we observed a more pronounced asymmetry with increasing diameter. Particularly, impact craters with larger D and d/D ratios (D > 7 km, d/D > 0.15) displayed an asymmetrical longitudinal distribution, aligning with predictions from the theoretical model. In the diameter range of 10 km–20km, for craters with d/D > 0.15, we observed that new crater influx occurring after 4.0 Ga years ago contributed little to this particular crater population. Therefore, we suggest that the cratering asymmetry was already present before 4.0 Ga. Due to the non-uniform ejecta from the Orientale Basin onto the highland regions, a significant number of smaller impact craters (1–5 km) have degraded or disappeared in the leading region, thereby diminishing the manifestation of the cratering asymmetry. The pronounced asymmetry exhibited in our statistical results might suggest the existence of a significant population of low-velocity impactors in early impact period (>4Ga) around the cis-lunar space.
以往的研究通过对数量有限的新陨石坑的数值模拟和统计分析，为同步旋转引起的月球表面陨石坑不对称性提供了证据。在这项研究中，我们重新评估了月球高地（70°W, 60°N）到（70°E, 60°S）区域的陨石坑不对称性，使用了直径(D)从1到20 km的新陨石坑目录。通过利用深径比（d/ d）约束来排除退化陨石坑和次生陨石坑的干扰，我们观察到d/ d >陨石坑的显著不对称性；0.15. 此外，利用大直径陨石坑(D >；随着直径的增加，我们观察到更明显的不对称性。特别是D和D /D比较大的陨石坑(D >；7公里，d/ d >；0.15)显示出不对称的纵向分布，与理论模型的预测一致。在直径10 ~ 20km范围内，对于d/ d >的陨石坑；0.15，我们观察到，在4.0亿年前之后发生的新陨石坑涌入对这个特定的陨石坑数量贡献不大。因此，我们认为陨石坑的不对称性在4.0 Ga之前就已经存在了。由于来自Orientale盆地的不均匀喷射到高原地区，导致大量较小的陨石坑（1-5 km）在领先区域退化或消失，从而减少了陨石坑不对称的表现。我们的统计结果显示出明显的不对称性，这可能表明在撞击早期（>4Ga），在顺月空间周围存在大量的低速撞击体。
{"title":"Asymmetrical distribution of 1–20 km craters on the Moon","authors":"Chenxu Zhao , Zongyu Yue , Kaichang Di , Yutong Jia , Wing-Huen Ip , Yangting Lin , Bo Wu , Biao Wang , Bin Xie","doi":"10.1016/j.pss.2024.106015","DOIUrl":"10.1016/j.pss.2024.106015","url":null,"abstract":"<div><div>Previous studies have provided evidence for the synchronous rotation induced cratering asymmetry on lunar surface through numerical simulations and statistical analysis of a limited number of fresh craters. In this study, we reevaluated cratering asymmetry in lunar highland from (70°W, 60°N) to (70°E, 60°S) region using a new crater catalogue with diameters (D) ranging from 1 to 20 km. By utilizing a depth-to-diameter (d/D) ratio constraint to exclude the interference of degraded and secondary craters, we observed significant asymmetry in craters with d/D > 0.15. Moreover, leveraging the characteristic that larger diameter craters (D > 7 km) are less susceptible to degradation, we observed a more pronounced asymmetry with increasing diameter. Particularly, impact craters with larger D and d/D ratios (D > 7 km, d/D > 0.15) displayed an asymmetrical longitudinal distribution, aligning with predictions from the theoretical model. In the diameter range of 10 km–20km, for craters with d/D > 0.15, we observed that new crater influx occurring after 4.0 Ga years ago contributed little to this particular crater population. Therefore, we suggest that the cratering asymmetry was already present before 4.0 Ga. Due to the non-uniform ejecta from the Orientale Basin onto the highland regions, a significant number of smaller impact craters (1–5 km) have degraded or disappeared in the leading region, thereby diminishing the manifestation of the cratering asymmetry. The pronounced asymmetry exhibited in our statistical results might suggest the existence of a significant population of low-velocity impactors in early impact period (>4Ga) around the cis-lunar space.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"254 ","pages":"Article 106015"},"PeriodicalIF":1.8,"publicationDate":"2024-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142757209","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}
Pub Date : 2024-11-15DOI: 10.1016/j.pss.2024.105984
Takashi Ito , Arika Higuchi
We describe the result of our numerical orbit simulation which traces dynamical evolution of new comets coming from the Oort Cloud. We combine two dynamical models for this purpose. The first one is semi-analytic, and it models an evolving comet cloud under galactic tide and encounters with nearby stars. The second one numerically deals with planetary perturbation in the planetary region. Although our study does not include physical effects such as fading or disintegration of comets, we found that typical dynamical resident time of the comets in the planetary region is about years. We also found that the so-called planet barrier works when the initial orbital inclination of the comets is small. A numerical result concerning the temporary transition of the comets into other small body populations such as transneptunian objects or Centaurs is discussed.
{"title":"An estimate of resident time of the Oort Cloud new comets in planetary region","authors":"Takashi Ito , Arika Higuchi","doi":"10.1016/j.pss.2024.105984","DOIUrl":"10.1016/j.pss.2024.105984","url":null,"abstract":"<div><div>We describe the result of our numerical orbit simulation which traces dynamical evolution of new comets coming from the Oort Cloud. We combine two dynamical models for this purpose. The first one is semi-analytic, and it models an evolving comet cloud under galactic tide and encounters with nearby stars. The second one numerically deals with planetary perturbation in the planetary region. Although our study does not include physical effects such as fading or disintegration of comets, we found that typical dynamical resident time of the comets in the planetary region is about <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>8</mn></mrow></msup></mrow></math></span> years. We also found that the so-called planet barrier works when the initial orbital inclination of the comets is small. A numerical result concerning the temporary transition of the comets into other small body populations such as transneptunian objects or Centaurs is discussed.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"253 ","pages":"Article 105984"},"PeriodicalIF":1.8,"publicationDate":"2024-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142650870","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}
Pub Date : 2024-11-15DOI: 10.1016/j.pss.2024.105995
Wolf-Stefan Benedix , Sebastian Hegler , Christoph Statz , Ronny Hahnel , Dirk Plettemeier , Valérie Ciarletti
While ground penetrating radars have been extensively researched on Earth, the high-resolution exploration and imaging of the shallow subsurface of celestial bodies in our solar system is still in its early stages, with only a handful of systems capable of the task.
Designing high-resolution radar systems can be a complex task due to the large frequency bandwidth required by the antennas to achieve high vertical resolution. The WISDOM GPR, as part of the 2028 ExoMars mission, is a highly capable and challenging instrument in this context, given its fully-polarimetric setup and mission constraints on the operating environment, robustness, as well as mass and size budget.
This paper outlines the development and characterization process of the WISDOM antenna assembly, which can serve as a model for future radar systems. Furthermore, it presents the results of the antenna characterization as the foundation for instrument calibration and optimal radar sounding outcomes.
{"title":"The ExoMars 2028 WISDOM antenna assembly: Description and characterization","authors":"Wolf-Stefan Benedix , Sebastian Hegler , Christoph Statz , Ronny Hahnel , Dirk Plettemeier , Valérie Ciarletti","doi":"10.1016/j.pss.2024.105995","DOIUrl":"10.1016/j.pss.2024.105995","url":null,"abstract":"<div><div>While ground penetrating radars have been extensively researched on Earth, the high-resolution exploration and imaging of the shallow subsurface of celestial bodies in our solar system is still in its early stages, with only a handful of systems capable of the task.</div><div>Designing high-resolution radar systems can be a complex task due to the large frequency bandwidth required by the antennas to achieve high vertical resolution. The WISDOM GPR, as part of the 2028 ExoMars mission, is a highly capable and challenging instrument in this context, given its fully-polarimetric setup and mission constraints on the operating environment, robustness, as well as mass and size budget.</div><div>This paper outlines the development and characterization process of the WISDOM antenna assembly, which can serve as a model for future radar systems. Furthermore, it presents the results of the antenna characterization as the foundation for instrument calibration and optimal radar sounding outcomes.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"253 ","pages":"Article 105995"},"PeriodicalIF":1.8,"publicationDate":"2024-11-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142650871","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}
Pub Date : 2024-11-10DOI: 10.1016/j.pss.2024.105998
А.T. Basilevsky , S.S. Krasilnikov , Yuan Li
The photogeologic analysis of the ShadowCam images of the permanently shadowed floor and lower parts of inner slopes of the near-polar lunar crater Shoemaker confirmed the conclusion of Basilevsky and Li (2024)that the surface morphology of the Shoemaker floor is dominated by a population of small (D < 1 km) craters. Future studies hopefully will allow to describe the morphology and morphometry (especially d/D) of the decameter-scale craters seen in the ShadowCam images. The surface of the lower parts of inners slopes of crater Shoemaker, which are permanently shadowed, has the “elephant hide” texture, that is also typical for normally illuminated slopes. So, most issues of the surface morphology were found to be identical or very close to those in normally illuminated regions of the Moon. The new finding in permanently shadowed areas is the presence of lobate-rimmed craters, whose morphology is probably indicative of water ice in the target material.
{"title":"Photogeological analysis of ShadowCam images of the permanently shadowed floor of lunar crater Shoemaker","authors":"А.T. Basilevsky , S.S. Krasilnikov , Yuan Li","doi":"10.1016/j.pss.2024.105998","DOIUrl":"10.1016/j.pss.2024.105998","url":null,"abstract":"<div><div>The photogeologic analysis of the ShadowCam images of the permanently shadowed floor and lower parts of inner slopes of the near-polar lunar crater Shoemaker confirmed the conclusion of Basilevsky and Li (2024)that the surface morphology of the Shoemaker floor is dominated by a population of small (D < 1 km) craters. Future studies hopefully will allow to describe the morphology and morphometry (especially d/D) of the decameter-scale craters seen in the ShadowCam images. The surface of the lower parts of inners slopes of crater Shoemaker, which are permanently shadowed, has the “elephant hide” texture, that is also typical for normally illuminated slopes. So, most issues of the surface morphology were found to be identical or very close to those in normally illuminated regions of the Moon. The new finding in permanently shadowed areas is the presence of lobate-rimmed craters, whose morphology is probably indicative of water ice in the target material.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"254 ","pages":"Article 105998"},"PeriodicalIF":1.8,"publicationDate":"2024-11-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142654042","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}
Pub Date : 2024-11-09DOI: 10.1016/j.pss.2024.105997
A. Tullo , C. Re , G. Cremonese , E. Martellato , R. La Grassa , N. Thomas
The present study analyses the potential of pansharpening algorithms for planetary exploration studies, testing their performance with the 4-band images from the Colour and Stereo Surface Imaging System (CaSSIS) aboard the Exomars 2016 Trace Grace Orbiter (TGO) using HiRISE images from the Mars Reconnaissance Orbiter (MRO) mission as the base. Due to the lack of suitable open-source tools, a suite of scripts was developed to improve alignment between images and enable different component substitution (CS) pansharpening algorithms. The tools developed were tested on a database of images encompassing several regions of Mars to explore its vast diversity in colours, tones, and textures. Then, the resulting images were investigated using spectral and structural performance indices, comparing the results with the source images and the colour information from the HiRISE central channels.
The results show that a substantial number of the tested algorithms are more than suitable for data enhancement, showing a considerable improvement in the structural characteristics of the images without sacrificing their spectral characteristics. In detail, the Gram-Schmidt method, widely used in terrestrial pansharpening, turns out to be the best compromise among the tested algorithms. Regarding the other tested algorithms, GIHS and the MMSE Brovey, a modified version of the classic Brovey, show the most significant increase in structural properties, while GHPF and GHPM show the interesting ability to maintain virtually unchanged spectral conditions of the multispectral source data.
In addition, the analysis reveals the applicability of pansharpening at a ground resolution increment up to 18 times, from 4.5 up to 0.25 m/px, a broader range than is usually used in traditional pansharpening.
{"title":"Performance evaluation of pansharpening for planetary exploration: A case study on the implementation of TGO CaSSIS with MRO HiRISE","authors":"A. Tullo , C. Re , G. Cremonese , E. Martellato , R. La Grassa , N. Thomas","doi":"10.1016/j.pss.2024.105997","DOIUrl":"10.1016/j.pss.2024.105997","url":null,"abstract":"<div><div>The present study analyses the potential of pansharpening algorithms for planetary exploration studies, testing their performance with the 4-band images from the Colour and Stereo Surface Imaging System (CaSSIS) aboard the Exomars 2016 Trace Grace Orbiter (TGO) using HiRISE images from the Mars Reconnaissance Orbiter (MRO) mission as the base. Due to the lack of suitable open-source tools, a suite of scripts was developed to improve alignment between images and enable different component substitution (CS) pansharpening algorithms. The tools developed were tested on a database of images encompassing several regions of Mars to explore its vast diversity in colours, tones, and textures. Then, the resulting images were investigated using spectral and structural performance indices, comparing the results with the source images and the colour information from the HiRISE central channels.</div><div>The results show that a substantial number of the tested algorithms are more than suitable for data enhancement, showing a considerable improvement in the structural characteristics of the images without sacrificing their spectral characteristics. In detail, the Gram-Schmidt method, widely used in terrestrial pansharpening, turns out to be the best compromise among the tested algorithms. Regarding the other tested algorithms, GIHS and the MMSE Brovey, a modified version of the classic Brovey, show the most significant increase in structural properties, while GHPF and GHPM show the interesting ability to maintain virtually unchanged spectral conditions of the multispectral source data.</div><div>In addition, the analysis reveals the applicability of pansharpening at a ground resolution increment up to 18 times, from 4.5 up to 0.25 m/px, a broader range than is usually used in traditional pansharpening.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"254 ","pages":"Article 105997"},"PeriodicalIF":1.8,"publicationDate":"2024-11-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142654041","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}
Halotrichite [FeAl2(SO4)4·22(H2O)] is a rare secondary sulfate mineral with its occurrence confined within the sulfide weathering zones. In the South Kerala Sedimentary Basin (SKSB) of SW India, halotrichite, here reported for the first time, is associated with an organic matter (OM)-rich carbonaceous clay layer. Field investigation revealed the prevalence of acid rock drainage (ARD) conditions similar to Martian analogue sites like Rio Tinto. The OM-layer is associated with pyrite forming substratum and Al-rich leachate associated with the Youngest Toba Tuff (YTT) cryptotephra layer. Oxidation of these units results in the formation of halotrichite, which is temporally restricted only to the dry season when the water table lowers and the OM-layer is exposed to air. X-Ray Diffraction (XRD) results for halotrichite show the presence of Al and Fe(II) sulfates. Energy Dispersive X-ray Spectroscopy (EDS) ruled out the existence of pickeringite, the Mg end-member of halotrichite-pickeringite series. XRD results for the OM-layer indicate the presence of kaolinite, quartz, goethite, and lepidocrocite. Hyperspectral analysis of the clay samples confirms that halotrichite is associated with goethite, lepidocrocite, kaolinite, and smectite. Fourier Transform Infrared Spectroscopy (FTIR) analysis revealed the major constituent of the clay sample as kaolinite with traces of quartz, smectite, and OM. Raman spectrum of halotrichite shows the symmetric stretching vibration of SO42− bonded to Fe2+. Association of halotrichite with Fe, Al, and S-rich minerals is also inferred by the study of Raman spectrum of the host clay. Co-existence of halotrichite, goethite, lepidocrocite, and phyllosilicates in the study area is similar to the mineral assemblage found along the Rio Tinto River. On Mars, halotrichite is associated with the layered sulfate deposits, such as those in Valles Marineris and Meridiani Planum, and is categorized as a polyhydrated sulfate. Hence, this study on the halotrichite mineralization in the SKSB can supplement the attempts on deciphering the deposition and formation environment of similar mineralization on Mars.
光卤石[FeAl2(SO4)4-22(H2O)]是一种罕见的次生硫酸盐矿物，只出现在硫化物风化带中。在印度西南部的南喀拉拉邦沉积盆地（SKSB），光卤石首次与富含有机质（OM）的碳质粘土层伴生。实地调查显示，酸性岩石排水（ARD）条件与力拓等火星类似地点相似。OM 层与黄铁矿形成的基底层以及与最年轻的多巴凝灰岩（YTT）隐晶质层相关的富铝浸出液有关。这些单元的氧化作用会形成卤黄铁矿，而卤黄铁矿在时间上仅限于旱季，因为旱季时地下水位降低，OM 层暴露在空气中。光卤石的 X 射线衍射（XRD）结果显示存在铝和硫酸铁（II）。能量色散 X 射线光谱（EDS）排除了光卤石-黝帘石系列的镁末端成员黝帘石的存在。OM 层的 XRD 结果表明存在高岭石、石英、网纹石和鳞片石。粘土样品的高光谱分析证实，光卤石与网纹石、鳞片石、高岭石和直闪石相关联。傅立叶变换红外光谱（FTIR）分析表明，粘土样品的主要成分是高岭石，还有微量的石英、直闪石和 OM。光卤石的拉曼光谱显示了与 Fe2+ 结合的 SO42- 的对称伸缩振动。通过对主粘土拉曼光谱的研究，还可以推断出光卤石与富含铁、铝和 S 的矿物的关联。在研究区域，光卤石、网纹石、鳞片石和植硅酸盐共存，这与在力拓河沿岸发现的矿物组合相似。在火星上，光卤石与层状硫酸盐矿床有关，如海洋谷（Valles Marineris）和子午线（Meridiani Planum）的硫酸盐矿床，被归类为多水合硫酸盐。因此，对 SKSB 中光卤石成矿作用的研究可以补充对火星上类似成矿作用的沉积和形成环境的解密尝试。
{"title":"Formation of halotrichite in the South Kerala Sedimentary Basin, SW India: Implications for Martian paleo-environmental studies","authors":"Kannan J. Prakash , Libiya M. Varghese , P.B. Hiral , Suresh Evna , V.R. Rani , K.S. Sajinkumar , V.J. Rajesh , G.K. Indu , Sneha Mukherjee , J.K. Tomson","doi":"10.1016/j.pss.2024.105999","DOIUrl":"10.1016/j.pss.2024.105999","url":null,"abstract":"<div><div>Halotrichite [FeAl<sub>2</sub>(SO<sub>4</sub>)<sub>4</sub>·22(H<sub>2</sub>O)] is a rare secondary sulfate mineral with its occurrence confined within the sulfide weathering zones. In the South Kerala Sedimentary Basin (SKSB) of SW India, halotrichite, here reported for the first time, is associated with an organic matter (OM)-rich carbonaceous clay layer. Field investigation revealed the prevalence of acid rock drainage (ARD) conditions similar to Martian analogue sites like Rio Tinto. The OM-layer is associated with pyrite forming substratum and Al-rich leachate associated with the Youngest Toba Tuff (YTT) cryptotephra layer. Oxidation of these units results in the formation of halotrichite, which is temporally restricted only to the dry season when the water table lowers and the OM-layer is exposed to air. X-Ray Diffraction (XRD) results for halotrichite show the presence of Al and Fe(II) sulfates. Energy Dispersive X-ray Spectroscopy (EDS) ruled out the existence of pickeringite, the Mg end-member of halotrichite-pickeringite series. XRD results for the OM-layer indicate the presence of kaolinite, quartz, goethite, and lepidocrocite. Hyperspectral analysis of the clay samples confirms that halotrichite is associated with goethite, lepidocrocite, kaolinite, and smectite. Fourier Transform Infrared Spectroscopy (FTIR) analysis revealed the major constituent of the clay sample as kaolinite with traces of quartz, smectite, and OM. Raman spectrum of halotrichite shows the symmetric stretching vibration of SO<sub>4</sub><sup>2−</sup> bonded to Fe<sup>2+</sup>. Association of halotrichite with Fe, Al, and S-rich minerals is also inferred by the study of Raman spectrum of the host clay. Co-existence of halotrichite, goethite, lepidocrocite, and phyllosilicates in the study area is similar to the mineral assemblage found along the Rio Tinto River. On Mars, halotrichite is associated with the layered sulfate deposits, such as those in Valles Marineris and Meridiani Planum, and is categorized as a polyhydrated sulfate. Hence, this study on the halotrichite mineralization in the SKSB can supplement the attempts on deciphering the deposition and formation environment of similar mineralization on Mars.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"254 ","pages":"Article 105999"},"PeriodicalIF":1.8,"publicationDate":"2024-11-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142654040","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}
Pub Date : 2024-10-22DOI: 10.1016/j.pss.2024.105985
Thomas Pierron, François Forget, Ehouarn Millour, Antoine Bierjon
Because of the high amount of dust in the Martian atmosphere, solar panels of landers and rovers on Mars get covered by dust in the course of their mission. This accumulation significantly decreases the available power over sols. During some missions, winds were able to blow the dust away. These ”dust cleaning events”, as they are called, were followed by an increase of the electrical current produced by the solar arrays. However, the Insight Lander solar panels were never cleaned and the mission died of dust accumulation. In order to better predict the evolution of available power produced by solar panels in the Martian conditions, this paper proposes a model of dust accumulation in which the solar flux under the accumulated dust layer is computed taking into account a full radiative transfer in the atmosphere and in the dust layer accumulated on the panel. This work uses several missions observation data to validate this model.
{"title":"Power attenuation of Martian rovers and landers solar panels due to dust deposition","authors":"Thomas Pierron, François Forget, Ehouarn Millour, Antoine Bierjon","doi":"10.1016/j.pss.2024.105985","DOIUrl":"10.1016/j.pss.2024.105985","url":null,"abstract":"<div><div>Because of the high amount of dust in the Martian atmosphere, solar panels of landers and rovers on Mars get covered by dust in the course of their mission. This accumulation significantly decreases the available power over sols. During some missions, winds were able to blow the dust away. These ”dust cleaning events”, as they are called, were followed by an increase of the electrical current produced by the solar arrays. However, the Insight Lander solar panels were never cleaned and the mission died of dust accumulation. In order to better predict the evolution of available power produced by solar panels in the Martian conditions, this paper proposes a model of dust accumulation in which the solar flux under the accumulated dust layer is computed taking into account a full radiative transfer in the atmosphere and in the dust layer accumulated on the panel. This work uses several missions observation data to validate this model.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":"253 ","pages":"Article 105985"},"PeriodicalIF":1.8,"publicationDate":"2024-10-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142551898","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}
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