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Power attenuation of Martian rovers and landers solar panels due to dust deposition 火星车和着陆器太阳能电池板因灰尘沉积而导致功率衰减
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-22 DOI: 10.1016/j.pss.2024.105985
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.
由于火星大气中含有大量灰尘,火星上的着陆器和漫游车的太阳能电池板在执行任务的过程中会被灰尘覆盖。这些灰尘的积累大大降低了太阳能电池板的可用功率。在某些任务中,风能够将灰尘吹走。这些所谓的 "灰尘清理事件 "之后,太阳能电池阵列产生的电流会增加。然而,"洞察号 "着陆器的太阳能电池板从未清洗过,这次任务也因灰尘堆积而失败。为了更好地预测太阳能电池板在火星条件下产生的可用功率的变化,本文提出了一个灰尘积聚模型,在该模型中,计算了积聚灰尘层下的太阳通量,并考虑了大气层和电池板上积聚的灰尘层中的完全辐射传递。这项工作利用几个任务的观测数据来验证这一模型。
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引用次数: 0
The thermal impact of the self-heating effect on airless bodies. The case of Mercury’s north polar craters 自热效应对无空气天体的热影响。水星北极陨石坑的情况
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-11 DOI: 10.1016/j.pss.2024.105983
Thermal models are essential for studying airless planetary surfaces, as the interaction between topography and thermophysical properties plays a crucial role in determining a surface’s response to localized illumination. Accurate temperature distribution calculations require a comprehensive investigation of sunlight scattering, a process that, despite its computational challenges, cannot be overlooked, especially when high resolution is necessary. Furthermore, thermal analysis is fundamental for assessing the stability of volatiles in polar regions. In this study, we introduce a novel approach by discretizing the Sun into 100 individual elements, allowing for a highly precise simulation of solar flux—an innovation crucial for accurately capturing temperature distributions in Mercury’s polar craters, given the planet’s proximity to the Sun. This level of discretization significantly enhances the accuracy of the thermal model, ensuring a more realistic depiction of how sunlight interacts with crater topography. We developed a dual-model approach that simulates both direct solar illumination and its scattering on two craters, Laxness and Fuller, located at Mercury’s north pole. The illumination and thermal model predict temperature distribution and heat transfer based on the material’s thermal properties and topography. The study examines the interaction between direct sunlight, causing localized heating, and scattered light, which influences the thermal response of surface materials. Detailed illumination maps and temperature profiles were generated over two Hermean years, revealing the significant impact of the self-heating effect on temperature distribution. The results show that specific regions experience indirect solar flux due to the craters’ morphology, particularly in permanently shadowed regions (PSRs) that are heated exclusively by scattered radiation. Maximum temperature profiles for the Laxness and Fuller craters show a substantial temperature increase within PSRs compared to areas exposed to direct illumination. However, while self-heating does not affect the stability of water ice in the Laxness crater, in the Fuller crater, a section within the radar-bright material reaches temperatures of up to 210 K, potentially threatening the stability of water ice. Further investigation with the onboard SIMBIO-SYS instrument on the BepiColombo mission will help to better understand the current state of these craters and their volatile deposits.
热模型对于研究无空气行星表面至关重要,因为地形和热物理性质之间的相互作用在决定表面对局部光照的响应方面起着至关重要的作用。精确的温度分布计算需要对太阳光散射进行全面研究,尽管这一过程在计算上具有挑战性,但不容忽视,尤其是在需要高分辨率的情况下。此外,热分析也是评估极地地区挥发物稳定性的基础。在这项研究中,我们引入了一种新方法,将太阳离散为 100 个单独的元素,从而能够高度精确地模拟太阳通量--鉴于水星靠近太阳,这种创新对于准确捕捉水星极地环形山的温度分布至关重要。这种离散化程度大大提高了热模型的准确性,确保更真实地描述阳光与陨石坑地形的相互作用。我们开发了一种双模型方法,模拟太阳直射及其对位于水星北极的拉克斯内斯和富勒这两个陨石坑的散射。照明和热模型根据材料的热特性和地形预测温度分布和热传导。这项研究考察了造成局部加热的直射阳光与影响表面材料热反应的散射光之间的相互作用。研究人员绘制了两个赫曼年的详细光照图和温度分布图,揭示了自加热效应对温度分布的重要影响。结果表明,由于陨石坑的形态,特定区域会受到间接太阳光通量的影响,特别是在完全由散射辐射加热的永久阴影区(PSRs)。拉克斯内斯陨石坑和富勒陨石坑的最高温度曲线显示,与受到直接照射的区域相比,PSRs 内的温度大幅上升。然而,虽然自热并不影响拉克斯内斯陨石坑中水冰的稳定性,但在富勒陨石坑中,雷达照射物质内的一段温度高达 210 K,有可能威胁到水冰的稳定性。利用贝皮科伦坡飞行任务上的星载 SIMBIO-SYS 仪器进行进一步调查,将有助于更好地了解这些陨石坑及其挥发性沉积物的现状。
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引用次数: 0
Comparison of volatiles evolving from selected highland and mare lunar regolith simulants during vacuum sintering 比较真空烧结过程中从选定的高原和泥质月球碎屑模拟物中挥发出来的挥发物
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-05 DOI: 10.1016/j.pss.2024.105982
Volatiles evolving from JSC-1A, NU-LHT-4M and CSM-LHT-1G lunar regolith simulants during in vacuo thermal processing were analyzed using mass spectrometry as a function of temperature. Two high-fidelity simulants, JSC-1A (mare) and NU-LHT-4M (highland), were compared to a newly developed CSM-LHT-1G highland simulant, modified to closely match lunar geochemistry. Large autogenous gas loads were observed for all investigated materials. Mineralogical knowledge was used to identify and attribute individual volatile species to reacting, transforming, or decomposing constituents (hydrates, carbonates, sulfates, sulfides, clays, etc.) of the respective regolith simulant in the self-generated gas environment. Cumulative mass losses for individual simulant components as a function of temperature were quantified using mass spectrometry in conjunction with thermogravimetric analysis. Investigation of the four components of CSM-LHT-1G – anorthosite, basalt, augite, and glass – aided the attribution of volatile species to specific compounds and their respective sources. The results showed significant decomposition of non-lunar phases present in the man-made regolith simulants below the typical glass crystallization temperatures, which paves the way to devising methods for enhancing the fidelity of the simulants. High gas loads and corrosive gases (HF and HCl) were recognized as potential hazards, pertaining to the development of large testbed facilities.
利用质谱仪分析了 JSC-1A、NU-LHT-4M 和 CSM-LHT-1G 月球碎屑模拟物在真空热处理过程中挥发出来的挥发物与温度的函数关系。将两种高保真模拟物 JSC-1A(裸砂)和 NU-LHT-4M(高原)与新开发的 CSM-LHT-1G 高原模拟物进行了比较,后者经过改良以密切匹配月球地球化学。在所有调查材料中都观察到了大量的自生气体负荷。矿物学知识被用来确定和归因于自生气体环境中相应的碎屑岩模拟物的反应、转化或分解成分(水合物、碳酸盐、硫酸盐、硫化物、粘土等)的个别挥发性物种。利用质谱法和热重分析法对模拟物各成分随温度变化的累积质量损失进行了量化。对 CSM-LHT-1G 的四种成分--正长岩、玄武岩、辉绿岩和玻璃--的研究有助于将挥发性物质归因于特定的化合物及其各自的来源。结果表明,人造雷公石模拟物中的非月相在典型的玻璃结晶温度以下发生了大量分解,这为设计提高模拟物真实性的方法铺平了道路。高气体负荷和腐蚀性气体(HF 和 HCl)被认为是潜在的危险,与大型试验台设施的开发有关。
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引用次数: 0
JunoPerijove 34: Update Ganymede 3D-control network and new DEMs study JunoPerijove 34:更新 Ganymede 3D 控制网络和新的 DEMs 研究
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-09-25 DOI: 10.1016/j.pss.2024.105981
During the Juno Perijove 34 the JunoCam acquired four RGB images of Ganymede. These images and updated SPICE kernel for spacecraft's trajectories were used to refine previous 3D-control point network (CPN). As a result, 4954 control points were measured 22,098 times with a minimum of 2 and a maximum of 16 observations per point, based on the 302 best available images from all missions (Voyagers, Galileo and Juno). After adjustment more than 86% of points have accuracy better than 3 km (>97% - better than 5 km). A new libration value for Ganymede 18ʺ is obtained. This updated CPN was used for compiling a new Ganymede global mosaic to support the planning of observations within the JUICE mission. New detailed local DEMs were obtained by stereovectorization for Enki Catena and Tros crater regions. In the Enki chain, the ratio d/D of the depth of craters to their diameter ranges from 0.049 to 0.089 and correlates with the area types (dark or light).
在 Juno Perijove 34 期间,JunoCam 获得了四幅木卫三的 RGB 图像。这些图像和更新的航天器轨迹 SPICE 内核被用来完善先前的三维控制点网络(CPN)。结果,根据所有飞行任务(旅行者号、伽利略号和朱诺号)提供的 302 幅最佳图像,对 4954 个控制点进行了 22 098 次测量,每个点的观测次数最少为 2 次,最多为 16 次。经过调整后,超过 86% 的点的精确度优于 3 千米(97% 优于 5 千米)。获得了甘尼米18ʺ的新天平校准值。更新后的 CPN 被用于编制新的 Ganymede 全球镶嵌图,以支持 JUICE 任务中的观测规划。通过对 Enki Catena 和 Tros 环形山区域进行立体矢量化,获得了新的详细局部 DEM。在恩基环形山链中,环形山深度与直径之比 d/D 在 0.049 至 0.089 之间,与区域类型(深色或浅色)相关。
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引用次数: 0
Morphological, hydrogeochemical and sedimentological analysis of hypersaline Sambhar Lake, India: An analog to understand evaporitic paleolake basins on Mars 印度桑巴尔超高盐湖的形态、水文地球化学和沉积学分析:了解火星上蒸发古湖盆地的类似物
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-09-18 DOI: 10.1016/j.pss.2024.105974
In the recent decade of astrobiological exploration of the Martian surface, there has been a shift from identifying habitable environments to finding markers indicative of biological activity. It requires a prior understanding of the physical and geochemical environment of the setting to decipher whether the conditions were conducive. Generally, quiescent surroundings of lacustrine basins are considered one of the best targets for the preservation of any biological signatures. However, due to logistical limitations, the geochemical information available is mostly restricted to small areas on the surficial level (or in the subsurface in case of layered deposits or impact craters) where sufficient satellite coverage is available and, in some areas, where rovers/landers have been deployed. In this context, terrestrial lacustrine basins offer valuable insights into the environment required for the formation of the minerals observed on the Martian surface.
This study was carried out within Sambhar Lake located in the arid/semiarid climatic zone within the Thar desert. It is a hypersaline playa that has undergone several cycles of desiccation and re-filling, sharing its climate-controlled history with that of several paleolakes on Mars. We conducted physicochemical analysis of the samples collected from the lake and its surrounding area and compared our results with samples from the Curiosity rover (at Gale crater) and to those of the studies carried out in basalt-rich parent settings of Iceland. Our results suggest that Sambhar Lake is a Na-Cl type brine with climate-driven hydrology. The shallow cores and rock samples indicated that the area is rich in evaporites. We propose that even the sites with different parent material may be crucial in understanding the geological evolution of paleolakes on Mars and that Sambhar is a great example to study tectono-geomorphic evolution and the climate-induced transition of a lacustrine basin to a playa. Additionally, the lake is also desirable to study extremophiles and their adaptation to changing environmental variables for future planetary missions, including but not limited to, Mars.
在最近十年对火星表面的天体生物学探索中,已经从确定宜居环境转向寻找表明生物活动的标记。这就要求事先了解环境的物理和地球化学环境,以破解条件是否有利。一般来说,湖沼盆地的静态环境被认为是保存任何生物特征的最佳目标之一。然而,由于后勤方面的限制,现有的地球化学信息大多局限于有足够卫星覆盖的表层小区域(或分层沉积或撞击坑的次表层),在某些地区,还部署了漫游车/登陆器。在这种情况下,陆地湖沼盆地为了解火星表面观察到的矿物形成所需的环境提供了宝贵的见解。这项研究是在位于塔尔沙漠干旱/半干旱气候区的桑巴尔湖内进行的。该湖是一个高盐水湖泊,经历了数次干燥和再充水周期,与火星上的几个古湖泊有着相同的气候控制历史。我们对从湖泊及其周边地区采集的样本进行了物理化学分析,并将分析结果与好奇号探测器(在盖尔陨石坑)采集的样本以及在冰岛富含玄武岩的母质环境中采集的样本进行了比较。我们的研究结果表明,桑巴尔湖是一种由气候驱动的 Na-Cl 型卤水。浅层岩心和岩石样本表明,该地区富含蒸发岩。我们认为,即使是母质不同的地点也可能对了解火星上古湖泊的地质演化至关重要,而桑巴尔湖则是研究构造地貌演化以及由气候引起的湖泊盆地向洼地过渡的一个很好的例子。此外,该湖也是研究嗜极生物及其对未来行星任务(包括但不限于火星)不断变化的环境变量的适应性的理想场所。
{"title":"Morphological, hydrogeochemical and sedimentological analysis of hypersaline Sambhar Lake, India: An analog to understand evaporitic paleolake basins on Mars","authors":"","doi":"10.1016/j.pss.2024.105974","DOIUrl":"10.1016/j.pss.2024.105974","url":null,"abstract":"<div><div>In the recent decade of astrobiological exploration of the Martian surface, there has been a shift from identifying habitable environments to finding markers indicative of biological activity. It requires a prior understanding of the physical and geochemical environment of the setting to decipher whether the conditions were conducive. Generally, quiescent surroundings of lacustrine basins are considered one of the best targets for the preservation of any biological signatures. However, due to logistical limitations, the geochemical information available is mostly restricted to small areas on the surficial level (or in the subsurface in case of layered deposits or impact craters) where sufficient satellite coverage is available and, in some areas, where rovers/landers have been deployed. In this context, terrestrial lacustrine basins offer valuable insights into the environment required for the formation of the minerals observed on the Martian surface.</div><div>This study was carried out within Sambhar Lake located in the arid/semiarid climatic zone within the Thar desert. It is a hypersaline playa that has undergone several cycles of desiccation and re-filling, sharing its climate-controlled history with that of several paleolakes on Mars. We conducted physicochemical analysis of the samples collected from the lake and its surrounding area and compared our results with samples from the Curiosity rover (at Gale crater) and to those of the studies carried out in basalt-rich parent settings of Iceland. Our results suggest that Sambhar Lake is a Na-Cl type brine with climate-driven hydrology. The shallow cores and rock samples indicated that the area is rich in evaporites. We propose that even the sites with different parent material may be crucial in understanding the geological evolution of paleolakes on Mars and that Sambhar is a great example to study tectono-geomorphic evolution and the climate-induced transition of a lacustrine basin to a playa. Additionally, the lake is also desirable to study extremophiles and their adaptation to changing environmental variables for future planetary missions, including but not limited to, Mars.</div></div>","PeriodicalId":20054,"journal":{"name":"Planetary and Space Science","volume":null,"pages":null},"PeriodicalIF":1.8,"publicationDate":"2024-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142311089","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}
引用次数: 0
A discussion on estimating small bodies taxonomies using phase curves results 关于利用相位曲线结果估算小天体分类的讨论
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-09-17 DOI: 10.1016/j.pss.2024.105970

Upcoming large multiwavelength photometric surveys will provide a leap in our understanding of small body populations, among other fields of modern astrophysics. Serendipitous observations of small bodies in different orbital locations allow us to study diverse phenomena related to how their surfaces scatter solar light.

In particular, multiple observations of the same object in different epochs permit us to construct their phase curves to obtain absolute magnitudes and phase coefficients. In this work, we tackle a series of long-used relationships associating these phase coefficients with the taxa of small bodies and suggest that some may need to be revised in the light of large-number statistics.

在现代天体物理学的其他领域中,即将进行的大型多波长测光勘测将为我们了解小天体群提供一个飞跃。对不同轨道位置的小天体的偶然观测,使我们能够研究与它们的表面如何散射太阳光有关的各种现象。特别是,在不同年代对同一天体的多次观测,使我们能够构建它们的相位曲线,从而获得绝对星等和相位系数。在这项工作中,我们处理了一系列长期使用的、将这些相位系数与小天体类群相关联的关系,并提出有些关系可能需要根据大数统计进行修订。
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引用次数: 0
Thermal extraction of water ice from the lunar surface II - vapor yields for an improved regolith model 月球表面水冰的热提取 II--改进的沉积岩模型的水汽产量
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-09-16 DOI: 10.1016/j.pss.2024.105973
<div><div>This work focuses on thermal water extraction on the lunar surface. We previously developed a three-dimensional finite element model (FEM) implementing heat and gas diffusion in the porous granular medium that is icy lunar regolith. Here, we present an improved version of this work in which we implemented a more realistic regolith model. In particular, we addressed previous model simplifications on regolith emissivity and porosity, water sublimation rate, as well as regolith and water ice thermal conductivity and permeability. Incorporating recent modeling and experimental work from the literature, we investigated the effect of these soil properties on the outcome of our simulations, with a particular interest in the yield of the thermal extraction process. Aiming at understanding what thermal water extraction would produce if heating the lunar surface directly, we also studied the effect of open borders on extraction yields.</div><div>We find that the crude icy regolith approximation we implemented in Paper I provided a lower estimation of water vapor yields upon heating. Overall and using the same heating methods (surface heating as well as inserted drills), our more accurate regolith model implementation extracted more water from the simulation volume. With this new model, we observed that extraction yields depended mostly on the ice content of the regolith, and to a lesser extent on the heating configuration (number of drills) and power. In two specific configurations, 16 and 25 drills at <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>4</mn></mrow></msup></mrow></math></span> W in 1%vol icy regolith, heating allowed the extraction of nearby ice, efficiently desiccating the entire simulation volume. Apart from these two cases, the highest extraction yields were obtained for <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>4</mn></mrow></msup></mrow></math></span> W surface heating of a volume with closed borders with values over 80%. In open border volumes, highest yields were around 70% achieved for the highest number of drills (16 and 25), at the highest power (<span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>4</mn></mrow></msup></mrow></math></span> W) in the regolith with the largest icy fraction. Extraction masses started being noticeable around a few minutes, but reaching most of the maximum possible yields took up to several days in some cases.</div><div>Defining an extraction efficiency by combining the yield and extraction times, we found that the best compromise between hardware complexity, time, and yield would be working in open border environments, using dense drill configurations in ice-rich regolith, and loose drill configurations in ice-poor regolith. In both cases, extraction efficiencies were similar at <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>2</mn></mrow></msup></mrow></math></span> W and <span><math><mrow><mn>1</mn><msup><mrow><mn>0
这项工作的重点是月球表面的热取水。我们之前开发了一个三维有限元模型(FEM),实现了多孔颗粒介质(即冰冷的月球残积岩)中的热量和气体扩散。在这里,我们提出了这一工作的改进版本,其中我们实施了一个更加逼真的碎屑岩模型。特别是,我们解决了以前模型中关于碎屑岩发射率和孔隙率、水升华速率以及碎屑岩和水冰导热性和渗透性的简化问题。结合最近的建模和文献实验工作,我们研究了这些土壤特性对模拟结果的影响,尤其关注热萃取过程的产量。为了了解如果直接加热月球表面,热萃取水会产生什么结果,我们还研究了开放边界对萃取产量的影响。我们发现,我们在论文 I 中实施的粗略冰质雷公石近似方法对加热后水蒸气产量的估计较低。总体而言,使用相同的加热方法(表面加热和插入钻头),我们更精确的岩石模型从模拟体积中提取了更多的水。通过这个新模型,我们观察到萃取率主要取决于岩石中的冰含量,其次才是加热配置(钻头数量)和功率。在两种特定配置下,即在体积为 1%的冰质残积岩中分别使用 104 瓦的 16 个和 25 个钻头,加热可以提取附近的冰,从而有效地使整个模拟体积干燥。除这两种情况外,对边界封闭的体积进行 104 W 表面加热时,提取率最高,超过 80%。在边界开阔的体积中,用最高功率(104 瓦)、最多钻头(16 个和 25 个)、冰成分最多的岩石中,最高提取率约为 70%。通过结合产量和提取时间来定义提取效率,我们发现硬件复杂性、时间和产量之间的最佳折中方案是在开放边界环境中工作,在富冰积岩中使用密集的钻头配置,在贫冰积岩中使用松散的钻头配置。在这两种情况下,每个钻头的功率分别为 102 瓦和 103 瓦,提取效率相近,这表明低功率方案比高功率方案能产生相似的结果。总之,我们的研究结果支持在未来的 ISRU 架构中进行热水提取的可行性。
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引用次数: 0
Isotopic fractionation of methane on Mars via diffusive separation in the subsurface 通过地表下的扩散分离实现火星上甲烷的同位素分馏
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-09-13 DOI: 10.1016/j.pss.2024.105971

Many processes have been identified in the Martian subsurface which may produce or release methane that eventually can be emitted into the atmosphere. Given the wide range of isotopic values for source carbon reported on Mars and the importance of atmospheric methane isotopologues as a tracer for subsurface processes, it is critical to quantify the level of isotopic fractionation that can occur during subsurface transport. On Earth, isotopic fractionation occurs when methane transport is dominated by Knudsen diffusion through small pores. However, unlike the Earth, on Mars the low atmospheric pressure and commensurate longer mean free path suggest that most subsurface transport of methane occurs in the Knudsen regime, amplifying this effect. Here, we report on simulations of diffusion through the martian subsurface and report on the level of fractionation that would be expected under two end-member scenarios. For Interplanetary Dust Particles (IDPs) incorporated in near-surface sediments in which methane is released quickly upon generation, atmospheric emissions of methane are expected to be representative of the reservoir isotopic ratio. However, for deeper sources in which methane accumulates as trapped gas, subsurface transport will result in depletions of 13CH4 compared to reservoir concentrations by approximately −31‰. Over time, both the reservoir and the emitted gas will evolve to become isotopically enriched in 13CH4 compared to a standard of constant isotopic ratio. This necessitates temporal measurements of emitted methane to understand the δ13C of the reservoir and depth of the release, preferably with hourly or better frequency. Finally, a seasonal cycle in δ13C with an amplitude of 5.3‰ is expected with adsorption acting to create small temporary reservoirs that are filled and emptied over the year by the subsurface thermal wave. This effect may provide a way to probe near-surface thermophysical properties.

火星地表下有许多过程可能会产生或释放甲烷,这些甲烷最终会排放到大气中。鉴于火星上报告的源碳同位素值范围很广,以及大气甲烷同位素作为地下过程示踪剂的重要性,量化地下迁移过程中可能发生的同位素分馏水平至关重要。在地球上,当甲烷传输主要是通过小孔隙进行克努森扩散时,就会发生同位素分馏。然而,与地球不同的是,火星上的低气压和相应的较长的平均自由路径表明,甲烷的大部分次表层迁移是在努森机制下发生的,从而放大了这种效应。在此,我们报告了通过火星地下扩散的模拟情况,并报告了在两种末端成员情况下的预期分馏水平。对于纳入近地表沉积物的行星际尘埃粒子(IDPs),甲烷在生成后会迅速释放,大气中的甲烷排放预计将代表储层的同位素比值。然而,对于甲烷作为滞留气体积聚的较深来源,地下传输将导致 13CH4 与储层浓度相比减少约 -31‰。随着时间的推移,与恒定同位素比的标准相比,储层和排放气体的 13CH4 都将发生同位素富集。这就需要对排放的甲烷进行时间测量,以了解储层和排放深度的 δ13C,测量频率最好为每小时或更高。最后,δ13C 的季节性周期振幅预计为 5.3‰,吸附作用会产生小型临时储层,这些储层在一年中会被地下热浪填满和排空。这种效应可为探测近地表热物理特性提供一种方法。
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引用次数: 0
Thermal modeling of the lunar South Pole: Application to the PROSPECT landing site 月球南极热建模:PROSPECT 着陆场的应用
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-09-11 DOI: 10.1016/j.pss.2024.105969

Water ice is distributed on the surface and in the subsurface of the Moon, as confirmed by observational data, and predicted by several numerical models. In this respect, the direct search for lunar water is the main objective of the ESA’s PROSPECT package, that aims to analyze a region of interest at the lunar South Pole. PROSPECT, originally on the Russian Luna 27, is now on the CLPS (Commercial Lunar Provider Service) “CP” 22 mission. In this work, we applied our 3-D FEM thermophysical model to investigate the landing site selected for the CP 22 mission, which is centred at −84.496°S, 31.588°E, and located on the Leibnitz Plateau and within an area of high elevation. The purpose of our model is to investigate regions of interest (ROI) on the lunar surface by working with the real topography at the scale of 5 m, by using the DEM (Digital Elevation Model) of the region. Since the lunar surface is characterized by topographic variations such as craters or boulders, a 3-D model is preferable over a 1-D numerical model. We produced temperature maps of the surface and 1-D temperature vs depth, as well as we produced illumination maps, computing also the indirect contribution. These simulations will provide a complete thermophysical vision of the landing site, offering a theoretical support to the researchers and engineers of the CP 22 mission, and of future lunar missions. In addition, this model can be applied to every site of the Moon surface and subsurface and, in general, to any airless body of the Solar System.

水冰分布在月球表面和地表下层,这一点已得到观测数据的证实和一些数值模型的预测。在这方面,直接寻找月球水是欧空局 PROSPECT 软件包的主要目标,该软件包旨在分析月球南极的一个相关区域。PROSPECT 最初由俄罗斯月球 27 号执行,现在由 CLPS(商业月球提供商服务)"CP "22 号任务执行。在这项工作中,我们应用我们的三维有限元热物理模型来研究为 CP 22 飞行任务选择的着陆点,该着陆点位于南纬-84.496°,东经 31.588°,位于莱布尼茨高原和高海拔地区。我们的模型旨在利用该区域的 DEM(数字高程模型),通过 5 米比例的真实地形,研究月球表面的兴趣区域(ROI)。由于月球表面存在陨石坑或巨石等地形变化,因此三维模型比一维数值模型更为理想。我们制作了表面温度图和一维温度与深度关系图,还制作了光照图,并计算了间接贡献。这些模拟将提供着陆点的完整热物理视图,为 CP 22 任务和未来月球任务的研究人员和工程师提供理论支持。此外,该模型还可应用于月球表面和地下的每个地点,一般来说,也可应用于太阳系的任何无空气天体。
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The Visual Monitoring Camera (VMC) on Mars Express: A new science instrument made from an old webcam orbiting Mars 火星快车上的视觉监控摄像机(VMC):利用火星轨道上的老式网络摄像头制作的新型科学仪器
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-09-11 DOI: 10.1016/j.pss.2024.105972

The Visual Monitoring Camera (VMC) is a small imaging instrument onboard Mars Express with a field of view of ∼40°x30°. The camera was initially intended to provide visual confirmation of the separation of the Beagle 2 lander and has similar technical specifications to a typical webcam of the 2000s. In 2007, a few years after the end of its original mission, VMC was turned on again to obtain full-disk images of Mars to be used for outreach purposes. As VMC obtained more images, the scientific potential of the camera became evident, and in 2018 the camera was given an upgraded status of a new scientific instrument, with science goals in the field of Martian atmosphere meteorology. The wide Field of View of the camera combined with the orbit of Mars Express enable the acquisition of full-disk images of the planet showing different local times, which for a long time has been rare among orbital missions around Mars. The small data volume of images also allows videos that show the atmospheric dynamics of dust and cloud systems to be obtained. This paper is intended to be the new reference paper for VMC as a scientific instrument, and thus provides an overview of the updated procedures to plan, command and execute science observations of the Martian atmosphere. These observations produce valuable science data that is calibrated and distributed to the community for scientific use.

视觉监测照相机(VMC)是火星快车上的一个小型成像仪器,视场角为 40°x30°。该相机最初的目的是为比格尔 2 号着陆器的分离提供视觉确认,其技术规格与 2000 年代的典型网络摄像头类似。2007 年,在其最初任务结束几年后,VMC 再次开启,以获取火星的全盘图像,用于外联目的。随着 VMC 获得更多图像,相机的科学潜力也逐渐显现,2018 年,相机被升级为新的科学仪器,其科学目标是火星大气气象学领域。相机的宽视场与火星快车的轨道相结合,能够获取显示不同局部时间的火星全盘图像,这在环绕火星的轨道任务中长期以来都是罕见的。由于图像数据量小,还可以获得显示尘埃和云系统大气动态的视频。本文旨在成为有关作为科学仪器的 VMC 的新参考文献,因此概述了计划、指挥和执行火星大气科学观测的最新程序。这些观测会产生宝贵的科学数据,这些数据经过校准后分发给社区,供科学界使用。
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