IF 2.5 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2024-11-06 DOI: 10.1016/j.icarus.2024.116368

Alison H. Graettinger, Julia Boyd, Joseph A. Nolan

Maar craters represent the top of a volcanic construct produced by subsurface explosive interactions between ground water/ice and rising magma. Recent comprehensive studies of terrestrial maars have established the commonality of complex maar crater geometries composed of overlapping circular components with a single near continuous outer rim. These distinctive geometries, and the availability of high spatial resolution visible imagery on Mars, provide an opportunity to identify and evaluate candidate maars on Mars. This study evaluated 49 closed depressions in Arena Colles and Nephentes/Amenthes based on their proximity to pitted cones of proposed volcanic origin. Across the two regions, 13 candidate maars were recognized for their similarity to terrestrial maars in absence of any exclusionary characteristics related to other formation processes such as butterfly ejecta around binary craters. The recognition of maars on Mars would provide additional proxies for the presence and range of depths for ground water and ice at the time of eruption. The diameter of the multiple overlapping circular components in maar craters can be used to provide first order estimates of the depths of the underlying diatreme as a proxy for depth of explosions and thus presence of water in the subsurface. Estimates based on the circular components of the 13 candidate maars recognized here indicate that water/ice depths at the time of formation would be between 0.6 and 4 km.

火山口是地下水/冰与上升岩浆之间的地下爆炸相互作用所产生的火山构造的顶部。最近对陆地火山口的全面研究已经确定了复杂的火山口几何形状的共性，这些几何形状由重叠的圆形部分和近乎连续的单一外缘组成。这些独特的几何形状以及火星上高空间分辨率的可见光图像为识别和评估火星上的候选火山口提供了机会。这项研究评估了阿瑞纳科林斯和奈芬特斯/阿门特斯的 49 个闭合凹陷，依据是这些凹陷是否靠近拟火山起源的凹陷锥。在这两个区域中，有 13 个候选火星环形山因其与陆地环形山的相似性而被确认，这些环形山没有任何与其他形成过程（如二元环形山周围的蝶形喷出物）有关的排他性特征。识别火星上的火山口将为火山爆发时地下水和冰的存在和深度范围提供额外的代用指标。火星环形山中多个重叠的圆形部分的直径可用来提供底层二迭熔岩深度的一阶估计值，作为爆炸深度的代用指标，从而确定地下是否有水。根据此处确认的 13 个候选火山口的圆形部分进行的估算表明，火山形成时的水/冰深度在 0.6 至 4 千米之间。

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引用次数: 0

3D morphometry of Martian craters from HRSC DEMs using a multi-scale semantic segmentation network and morphological analysis 利用多尺度语义分割网络和形态学分析，从 HRSC DEMs 得出火星陨石坑的三维形态测量结果

IF 2.5 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2024-11-04 DOI: 10.1016/j.icarus.2024.116358

Peiqi Ye , Rong Huang , Yusheng Xu , Wendi Li , Zhen Ye , Xiaohua Tong

The morphology of impact craters reveals the structure and composition of the Martian surface, especially the subsurface conditions and Martian geological history, which have increasing importance in Mars exploration missions. This work presents a 3D morphometric method for detecting and delineating Martian craters, and a 3D morphological analysis was conducted. Specifically, this work first focused on the segmentation of Martian craters. Based on the segmentation results, clustering of crater instances was then carried out. Finally, with the individual craters that were extracted, a morphological analysis involving the measurements of their diameter, depth, area, RMS height, rim height, circularity, and the statistics thereof was performed. Unlike previous studies, which have mainly used optical images and object detection approaches, this work regards crater extraction as a semantic segmentation task instead of an object detection task to better delineate the precise shape and boundary information. Digital elevation model (DEM) was utilized as primary data to directly obtain 3D information, which was converted into 3D point cloud format and fed to a multi-scale semantic segmentation network. The semantic segmentation results achieved an overall accuracy of 0.932 and mIOU of 0.871 on the test data. We automatically counted 63 craters in Noachis Terra and 40 craters in Terra Cimmeria. The 3D morphological measurements showed that 66% of the impact craters in the first region were larger than 10 km in diameter, while 50% of the impact craters in the second region were larger than 10 km. In both areas, craters could reach a maximum depth of 2000 m. With the proposed method, we can automatically conduct 3D morphological measurements of Martian craters with high efficiency that is improved by 15 times compared with that of manual crater analysis tools. The achieved 3D morphometric results can provide a reference and support for future research on Martian landforms.

撞击坑的形态揭示了火星表面的结构和组成，特别是地下条件和火星地质历史，在火星探测任务中具有越来越重要的意义。本研究提出了一种用于探测和划分火星撞击坑的三维形态测量方法，并进行了三维形态分析。具体来说，这项工作首先侧重于火星陨石坑的分割。然后根据分割结果对陨石坑实例进行聚类。最后，对提取出的单个陨石坑进行形态分析，包括测量其直径、深度、面积、均方根高度、边缘高度、圆度及其统计数据。与以往主要使用光学图像和物体检测方法的研究不同，这项工作将陨石坑提取视为语义分割任务，而不是物体检测任务，以便更好地划分精确的形状和边界信息。利用数字高程模型（DEM）作为原始数据，直接获取三维信息，并将其转换为三维点云格式，输入多尺度语义分割网络。在测试数据上，语义分割结果的总体准确率达到 0.932，mIOU 达到 0.871。我们自动统计了 Noachis Terra 的 63 个陨石坑和 Terra Cimmeria 的 40 个陨石坑。三维形态测量结果显示，第一个地区 66% 的撞击坑直径大于 10 千米，而第二个地区 50% 的撞击坑直径大于 10 千米。利用所提出的方法，我们可以自动对火星陨石坑进行三维形态测量，其效率比人工陨石坑分析工具提高了 15 倍。所获得的三维形态测量结果可为今后的火星地貌研究提供参考和支持。

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引用次数: 0

Maximum dust-to-gas mass flux ratio in spherically expanding dusty-gas flow 球形膨胀尘气流中尘埃与气体的最大质量通量比

IF 2.5 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2024-11-03 DOI: 10.1016/j.icarus.2024.116363

V.V. Zakharov , N.Y. Bykov , A. Rotundi , A.V. Rodionov , V. Della Corte , S.L. Ivanovski

In this paper, we consider the motion of a solid spherical particle in a spherically expanding gas flow as an elementary model of the gas-dust atmosphere of a comet. Based on the results of numerical simulations we propose an approximation for the terminal dust velocity and an estimate of the maximum dust-to-gas mass flux ratio (in a dusty-gas flow with the dust size distribution given by a power law) which is consistent with assumption of negligible impact of dust on the gas flow (frequently used in simulations of dusty gas flows).

在本文中，我们把固体球形粒子在球形膨胀气体流中的运动视为彗星气尘大气的基本模型。根据数值模拟的结果，我们提出了尘埃末端速度的近似值，并估算了尘埃与气体的最大质量通量比（在尘埃大小分布由幂律给出的尘埃-气体流中），该近似值与尘埃对气体流的影响可忽略不计的假设（常用于模拟尘埃气体流）是一致的。

引用次数: 0

Measurements of line parameters for 12C16O2 near λ = 1.05 μm by cavity ring-down spectrometer 利用空腔环降光谱仪测量 λ = 1.05 μm 附近 12C16O2 的线参数

IF 2.5 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2024-11-02 DOI: 10.1016/j.icarus.2024.116359

Tao Yang , Xianmei Qian , Qiang Liu , Wenyue Zhu , Hongliang Ma , Jianjie Zheng , Chaolong Cui , Xiaomei Jin , Jun Huang

The absorption spectra of ¹²C¹⁶O₂ within the wavenumber range of 9358–9648 cm⁻¹ have been precisely measured using a continuous-wave cavity ring-down spectrometer at room temperature. Employing synthetic gas mixtures comprising carbon dioxide, nitrogen, and argon, the line parameters, including line intensities and self-, N₂- and Ar- broadening coefficients have been retrieved in the 2003r-00001 (r = 1,2,3) bands. This retrieval process was facilitated by a multi-spectral fitting program that utilizes Voigt line profiles. A comparative analysis of our measured line intensities and self-broadening coefficients with those present in established databases, such as HITRAN2020, CDSD296, AMES-2021, and HITEMP2010, has been conducted. The line intensities and self-broadening coefficients for ¹²C¹⁶O₂ deviate by an average of less than 1 % from the values reported in the HITRAN2020 database. The J-dependence of N₂- and Ar- broadening coefficients has been investigated by comparing this work with experimental results and theoretical predictions from other vibrational bands. This research offers important experimental references for the improvement of computational models and the exploration of Venus and Mars.

利用连续波腔环降光谱仪在室温下精确测量了 12C16O2 在 9358-9648 cm-1 波长范围内的吸收光谱。利用由二氧化碳、氮气和氩气组成的合成气体混合物，对 2003r-00001 (r = 1,2,3) 波段中的线参数进行了检索，包括线强度和自、N2- 和氩气展宽系数。利用 Voigt 线剖面的多光谱拟合程序为这一检索过程提供了便利。我们将测得的线强度和自宽系数与现有数据库（如 HITRAN2020、CDSD296、AMES-2021 和 HITEMP2010）中的线强度和自宽系数进行了比较分析。12C16O2 的线强度和自展宽系数与 HITRAN2020 数据库中报告的数值平均偏差不到 1%。通过与实验结果和其他振动波段的理论预测进行比较，研究了 N2-和 Ar-展宽系数的 J 依赖性。这项研究为改进计算模型以及探索金星和火星提供了重要的实验参考。

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引用次数: 0

Detection of lunar water, hydroxyl ion and their diurnal changes from CHACE-2 orbiter observation 从CHACE-2轨道器观测中探测月球水、羟基离子及其昼夜变化

IF 2.5 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2024-10-31 DOI: 10.1016/j.icarus.2024.116365

Swastika Chakraborty , Barun Raychaudhuri , Tirtha Pratim Das , Saurabh Das , Moumita Roy

This work reports the spatial and diurnal variations of the number densities of lunar molecular water (H₂O), atomic mass unit (amu) 18 and hydroxyl (OH), amu 17 over low (0° to 30°), middle (31° to 60°) and high (61° to 80°) latitudinal regions of the lunar exosphere during the pre-sunrise, noon, sunset and midnight periods using the mass spectrometric data of CHandra's Atmospheric Composition Explorer-2 (CHACE-2) on board Chandrayaan-2, the second lunar mission developed in India. Both H₂O and OH exhibit, particularly in the low latitude regions, a trend of increasing number density after the sunrise and up to noon, followed by a decrease till sunset. An overall higher density of H₂O is obtained compared to the previous reports. The findings are justified in terms of the polar orbital height of the instrument and the duration of data procurement. The maximum number density for the low, middle and high latitudes reaches 5225 cm⁻³, 5135 cm⁻³ and 3747 cm⁻³, respectively. The corresponding OH abundances are found to be 5079 cm⁻³, 5565 cm⁻³ and 5720 cm⁻³. The diurnal variations of H₂O and OH and their comparisons, similar to those of the present report may provide suitable means for tracing the lunar water cycle. The CHACE-2 observations imply that the influence of magnetotail passage on volatiles like water is to be further quantified in future missions with other sensors.

这项工作报告了月球外大气层低纬度（0°至 30°）、中纬度（31°至 60°）和高纬度（61°至 80°）区域在日出前、正午、日落和午夜期间月球分子水（H2O）原子质量单位（amu）18 和羟基（OH）原子质量单位（amu）17 的数量密度的空间和昼夜变化、利用印度开发的第二个月球任务 Chandrayaan-2 号上的 CHandra's Atmospheric Composition Explorer-2 (CHACE-2) 的质谱数据，对日出前、正午、日落和午夜期间的月球外大气层进行了分析。特别是在低纬度地区，H2O 和 OH 的数量密度在日出后至正午前呈上升趋势，随后下降，直至日落。与以前的报告相比，H2O 的密度总体较高。从仪器的极轨道高度和数据采集的持续时间来看，这些发现都是合理的。低纬度、中纬度和高纬度的最大数量密度分别达到 5225 cm-3、5135 cm-3 和 3747 cm-3。相应的 OH 丰度分别为 5079 cm-3、5565 cm-3 和 5720 cm-3。与本报告类似，H2O 和 OH 的昼夜变化及其比较可为追踪月球水循环提供合适的方法。CHACE-2 的观测结果表明，磁尾通过对水等挥发物的影响需要在今后的飞行任务中利用其他传感器进一步量化。

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引用次数: 0

Large impact features on Ganymede and Callisto as revealed by geological mapping and morphometry 地质测绘和形态测量揭示的木卫三和卡利斯托大型撞击特征

IF 2.5 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2024-10-30 DOI: 10.1016/j.icarus.2024.116357

Oliver L. White , Jeffrey M. Moore , Paul M. Schenk , Donald G. Korycansky , Andrew J. Dombard , Martina L. Caussi , Kelsi N. Singer

The icy Galilean satellites are host to a broad range of impact feature morphologies. Hypotheses seeking to explain the diversity of these impact features consider the effects of impact melt, the physical state of the subsurface at the time of impact, and the impactor characteristics. As part of a larger effort to assess the role of these factors in the formation and evolution of these impact features, we have performed topographic and geological mapping of 19 large impact features on Ganymede and Callisto. These are divided into two main morphological groups: craters (subdivided into pit, dome, and anomalous dome craters), and penepalimpsests/palimpsests. The transitions from pit, dome, to anomalous dome craters appear to be size-dependent up to diameters of ∼170 km. The morphologies of pit and dome craters appear to be independent of their age or geologic context. The impacts that formed them only affected a cold, rigid ice layer, with the development of pits and raised annuli on their floors possibly stemming from the evolution of a pocket of impact melt. The subdued rims and floors of anomalous dome craters indicate the increasing effect of a weak, warm ice layer on impact feature morphology with increasing size, but their prominent annuli and pits indicate that mobilization of impact melt is also a factor. The very low topographic relief of older penepalimpsests and palimpsests indicates that their impacts penetrated the ice shell to mobilize very large volumes of pre-existing liquid from a subsurface layer, with little contribution to the final feature morphology from impact melt. Penepalimpsests are distinguished from palimpsests by the higher frequency of concentric ridges within their interiors, indicating a generally more robust state of the subsurface that could better support the rotation and uplift of solid material during impact, even if a crater-like depression could not be supported. A few impact features seem to be transitional between anomalous dome craters and penepalimpsests, and the overlap of anomalous dome craters, penepalimpsests, and palimpsests in terms of diameter as well as age indicates that impactor size and subsurface properties over time are major factors in determining which of these morphologies emerges.

冰冷的伽利略卫星上有各种各样的撞击特征形态。试图解释这些撞击特征多样性的假设考虑了撞击熔体的影响、撞击时地下的物理状态以及撞击者的特征。为了评估这些因素在这些撞击地貌的形成和演变过程中所起的作用，我们对木卫三和卡利斯托上的19个大型撞击地貌进行了地形和地质测绘。这些地貌分为两大形态组：陨石坑（细分为坑状、穹状和异常穹状陨石坑）和半椭球体/椭球体。从凹坑、圆顶到异常圆顶陨石坑的过渡似乎与直径在170千米以下的陨石坑的大小有关。坑状和穹状陨石坑的形态似乎与它们的年龄或地质背景无关。形成这些陨石坑的撞击只影响到冰冷坚硬的冰层，陨石坑底部凹坑和凸起的环状结构可能是由撞击熔融物形成的。异常穹隆陨石坑的边缘和坑底较低，这表明随着体积的增大，弱温冰层对撞击地貌形态的影响越来越大，但其突出的环状凹坑表明撞击熔融物的移动也是一个因素。较早的半侏罗纪火山口和重侏罗纪火山口的地形起伏很低，这表明它们的撞击穿透了冰壳，从地表层下动员了大量原有的液体，而撞击融化物对最终地貌形态的影响很小。半坍方地貌与重坍方地貌的区别在于其内部同心脊的出现频率较高，这表明次表层一般较为坚固，能够更好地支持固体物质在撞击过程中的旋转和隆起，即使无法支持类似陨石坑的凹陷。一些撞击特征似乎是异常穹隆陨石坑和半侏罗纪陨石坑之间的过渡，异常穹隆陨石坑、半侏罗纪陨石坑和垛状陨石坑在直径和年龄上的重叠表明，撞击物的大小和随时间变化的次表层性质是决定这些形态中哪一种出现的主要因素。

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引用次数: 0

Baroclinic waves observed on Mars from InSight data 根据 InSight 数据在火星上观测到的巴洛克波

IF 2.5 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2024-10-29 DOI: 10.1016/j.icarus.2024.116361

Victor Corchete

Baroclinic waves has been observed in the Martian atmosphere, and their periods have been calculated by means of spectral analysis of the pressure and wind velocity data, provided by the InSight mission for the time periods of the spring and winter seasons. For the spring time, the pressure spectrum shows a peak at the frequency of 0.246 (4 sol). For the winter time, the spectra of the pressure and wind velocity show a dominant peak at the frequency of ∼0.15 (6.7 sol), and a smaller peak at the frequency of ∼0.435 (2.3 sol). The results of this study are consistent with those determined in previous studies from spectral analysis of the Viking 2 data, and it is expected that a further analysis of the results determined in this study will provide a valuable insight into the seasonal changes of the atmospheric structure and circulation, which may be useful to fit General Circulation Models of the Martian atmosphere. However, a general understanding of Martian baroclinic phenomena only will be achieved with a combination of data from multiple Martian midlatitude stations in future missions.

在火星大气中观测到了巴罗克林波，并通过对 InSight 飞行任务提供的春季和冬季压力和风速数据进行频谱分析，计算出了它们的周期。在春季，压力频谱显示出频率为 0.246（4 索尔）的峰值。在冬季，压力和风速频谱在频率 ∼0.15 （6.7 个太阳）处显示出一个主峰，在频率 ∼0.435 （2.3 个太阳）处显示出一个较小的峰值。本研究的结果与以往研究中通过对海盗 2 号数据进行光谱分析而确定的结果相一致，预计对本研究确定的结果进行进一步分析将对大气结构和环流的季节性变化提供有价值的见解，这可能有助于拟合火星大气的一般环流模型。不过，只有在今后的飞行任务中结合多个火星中纬度站的数据，才能对火星的气压现象有一个总体的了解。

引用次数: 0

Iron isotopes of Chang'e-5 soil and mineral components: Implications for post-eruption processes on lunar surface 嫦娥五号土壤和矿物成分的铁同位素：对月球表面爆发后过程的影响

IF 2.5 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2024-10-29 DOI: 10.1016/j.icarus.2024.116362

Yiheng Li , Zaicong Wang , Yuqi Qian , Wen Zhang , Yantong Feng , Hong Liu , Keqing Zong , Qi He , Zhenbing She , Xiang Wu , Ming Li , Zhaochu Hu , Long Xiao , Yang Li , Frederic Moynier

Due to rapid magma cooling and extensive space weathering, significant disequilibrium crystallization and secondary modification widely occur in lunar mare basalt after its eruption on the lunar surface. In this study, we conducted bulk and in-situ Fe isotope analyses to investigate the post-eruption processes on Chang'e-5 (CE-5) samples. The CE-5 soil shows a minor elevation of δ⁵⁶Fe value (∼0.05 ‰) relative to the CE-5 basalt clasts. Correlations between Ni and Cu contents with δ⁵⁶Fe values suggest that the minor increase in the δ⁵⁶Fe from the CE-5 basalt to soil primarily occurred during evaporation caused by meteorite impacts. Such isotopic variation between CE-5 basalt and soils is notably lower than what is observed for Apollo samples and reflects the low maturity of CE-5 soils. This is consistent with the low Is/FeO value constrained by magnetic approaches. Therefore, measuring the δ⁵⁶Fe values of lunar soil is suitable to evaluate the degrees of maturity for lunar soils due to space weathering. In-situ analyses of δ⁵⁶Fe reveal significant variations in different grains of olivine (δ⁵⁶Fe: −0.57 to −0.17 ‰) and ilmenite (−0.06 to +0.42 ‰) and also in their interior (mainly for olivine). These δ⁵⁶Fe variations in minerals can be ascribed to the disequilibrium crystallization of lava flow and fast cooling, which is consistent with conclusions based on petrologic observations such as its extensive differentiation and silicate liquid immiscibility. Therefore, the post-eruption processes on the lunar surface could lead to significant variations in isotopic compositions at different scales of basalts, which in turn record the history of late-stage magma evolution and space weathering on the lunar surface.

由于岩浆的快速冷却和广泛的空间风化作用，月壤玄武岩在月面喷发后普遍发生了严重的不平衡结晶和二次改造。在本研究中，我们对嫦娥五号（CE-5）样品进行了散装和原位铁同位素分析，以研究其喷发后的过程。与嫦娥五号玄武岩碎屑相比，嫦娥五号土壤中的δ56Fe值略有升高（∼0.05 ‰）。镍和铜含量与δ56Fe值之间的相关性表明，从CE-5玄武岩到土壤的δ56Fe的微小增加主要发生在陨石撞击引起的蒸发过程中。CE-5 玄武岩和土壤之间的这种同位素变化明显低于阿波罗样本，反映了 CE-5 土壤的低成熟度。这与磁性方法得出的低Is/FeO值是一致的。因此，测量月球土壤的 δ56Fe 值适用于评估空间风化造成的月球土壤成熟度。δ56Fe的原位分析显示，橄榄石（δ56Fe：-0.57至-0.17‰）和钛铁矿（-0.06至+0.42‰）的不同晶粒及其内部（主要是橄榄石）存在显著差异。矿物中的δ56Fe变化可归因于熔岩流的不平衡结晶和快速冷却，这与根据岩石学观察得出的结论是一致的，如熔岩流的广泛分异和硅酸盐液的不溶性。因此，月球表面爆发后的过程可能导致不同尺度玄武岩同位素组成的显著变化，进而记录了月球表面后期岩浆演化和空间风化的历史。

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引用次数: 0

Three-dimensional modeling of Ganymede’s Chapman–Ferraro magnetic field and its role in subsurface ocean induction 木卫三查普曼-费拉罗磁场的三维建模及其在地表下海洋感应中的作用

IF 2.5 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2024-10-28 DOI: 10.1016/j.icarus.2024.116356

Nawapat Kaweeyanun , Adam Masters

In April 2023, the Jupiter Icy Moons Explorer (Juice) began its journey to orbit Jupiter’s largest and only magnetic moon, Ganymede. Part of the mission’s objectives aim to verify existence of the moon’s subsurface ocean and determine its structure through its induced response to external excitation by periodically varying magnetic field. Known contributions to the excitation are those from Jupiter’s dipole (at synodic period) and quadrupole (at half-synodic period) variations, and Ganymede’s inclined eccentric orbit around Jupiter (at orbital period). We propose that Ganymede’s magnetopause, where the Chapman–Ferraro (C–F) magnetic field arises from local currents, also contributes to subsurface ocean induction. This article introduces the first three-dimensional model of the C–F field and its outputs at Ganymede’s subsurface ocean and larger magnetosphere. The field is shown to be non-uniform — strongest near upstream Ganymede’s subflow region and gradually weakening away from it. Magnetopause asymmetry due to the Jovian guide field results in largely synodic variation of the C–F field, with exceptions near Ganymede’s equator and subflow meridian where asymmetry effects are minimal and the variations are half-synodic. The C–F field amplitude is of general order

\sim 50

nT, which is significant relative to excitation from the Jovian field. Comparisons to Galileo data and magnetohydrodynamic simulation results suggest the model is useful, therefore the magnetopause effects must be considered in future induction modeling of Ganymede’s subsurface ocean ahead of the Juice mission.

2023 年 4 月，木星冰月探测器（Juice）开始了环绕木星最大也是唯一的磁性卫星-- 木卫三（Ganymede）的旅程。此次任务的部分目标是验证该卫星是否存在地表下海洋，并通过其对周期性变化磁场的外部激励的感应反应确定其结构。已知的激励作用来自木星的偶极（同步周期）和四极（半同步周期）变化，以及木卫三围绕木星的倾斜偏心轨道（轨道周期）。我们提出，木卫三的磁极顶（Chapman-Ferraro（C-F）磁场产生于当地海流）也是造成地表下海洋感应的原因。本文首次介绍了 C-F 磁场的三维模型及其在木卫三次表层海洋和较大磁层的输出。研究表明，该磁场是不均匀的--在甘耶米德子流区上游附近最强，远离子流区后逐渐减弱。木卫二导磁场造成的磁极不对称导致了 C-F 磁场的大体同步变化，但在甘耶米德赤道和亚气流子午线附近例外，那里的不对称影响最小，变化为半同步。C-F场的振幅一般为50 nT，相对于来自木卫二场的激励来说是相当大的。与伽利略数据和磁流体动力学模拟结果的比较表明，该模型是有用的，因此，在 "朱伊斯 "任务之前，在对甘耶米底层海洋进行感应建模时，必须考虑磁极效应。

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引用次数: 0

Seasonal and interannual variability of the water vapor vertical distribution in the Martian lower atmosphere 火星低层大气中水汽垂直分布的季节性和年际可变性

IF 2.5 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2024-10-28 DOI: 10.1016/j.icarus.2024.116360

Alexey A. Pankine , Timothy H. McConnochie , Michael D. Smith

We apply a novel method to retrieve water vapor vertical distributions in the Martian atmosphere to spectra collected by the Mars Global Surveyor (MGS) Thermal Emission Spectrometer (TES). The new method exploits differences in sensitivity of the daytime and nighttime TES nadir spectra to water vapor content in different parts of the lower atmosphere (0–40 km). Based on the test retrievals from simulated environments, vertical profiles of water vapor can be retrieved with accuracy ∼20–40 % depending on the season and altitude above surface. Retrievals from observations collected by the MGS TES between L_s = 135° in MY24 and L_s = 75° in MY27 enable exploration of the seasonal and interannual variabilities of the vertical distribution of water vapor. Retrieved vapor distributions and their seasonal variability are generally consistent with those predicted by a numerical circulation model. Vapor is concentrated near the surface in the northern polar region and the mid-latitudes during the northern summer (L_s = 90°). During the southern summer (L_s = 270°) vapor extends higher in the atmosphere in the southern polar region, reflecting both sublimation of the seasonal surface ice and atmospheric transport by the upper branch of the southern Hadley cell. During both equinoxes (L_s = 0° and L_s = 180°) vapor is found in the lower part of the tropical atmosphere. At the same time the retrieved vertical distributions exhibit notable interannual variability. Following the global dust storm of MY25, vapor is confined to lower altitudes in the southern polar region during the southern summer. During the southern spring in MY26 (L_s = 180°-270°) vapor extends higher in the atmosphere and mixing ratios increase faster with height at the equator and in the northern tropics. These examples suggest that Martian atmosphere may experience interannual changes in the atmospheric transport, some of which could be in response to global dust storm events.

我们对火星全球勘测器（MGS）热辐射光谱仪（TES）收集的光谱采用了一种新方法来检索火星大气中的水汽垂直分布。新方法利用了白天和夜间 TES 天底光谱对低层大气（0-40 公里）不同部分水汽含量敏感度的差异。根据模拟环境的测试检索，水汽垂直剖面的检索精度可达 20-40 %，具体取决于季节和地面高度。从 MGS TES 在 MY24 的 Ls = 135° 和 MY27 的 Ls = 75° 之间收集的观测数据中检索水汽，可以探索水汽垂直分布的季节和年际变化。检索到的水汽分布及其季节变化与数值环流模式的预测基本一致。在北部夏季（Ls = 90°），水汽主要集中在北极地区和中纬度地区的地表附近。在南半球夏季（Ls = 270°），水汽在南极地区大气中的位置较高，这既反映了季节性地表冰的升华，也反映了南哈德利小区上支的大气输送。在两个春分（Ls = 0° 和 Ls = 180°）期间，热带大气的下部都有水汽。同时，检索到的垂直分布表现出明显的年际变化。25 年全球沙尘暴之后，水汽在南部夏季被限制在南极地区的较低高度。在 MY26 的南部春季（Ls = 180°-270°），水汽在大气中延伸到更高的位置，在赤道和北部热带地区，混合比随着高度的增加而加快。这些例子表明，火星大气可能会经历大气传输的年际变化，其中一些可能是对全球沙尘暴事件的响应。

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