IF 3 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2026-05-15 Epub Date: 2026-01-21 DOI: 10.1016/j.icarus.2026.116949

Pascal Rannou , Bruno de Batz de Trenquelléon , Sébastien Rodriguez , Benoît Seignovert

The Cassini orbiter around Saturn monitored Titan with multiple instruments 13 years, between 2004 to 2017. This is about half of a Titan year and this period included a major seasonal change at the North Spring Equinox (NSE) in 2009 that could be observed. The Visual and Infrared Mapping Spectrometer (VIMS) onboard Cassini produced a large amount of observations of Titan generally presented under the form of spectro-images. The observations with the IR part of VIMS detector are taken in a spectral range between 0.88 to

5.12 μ m

and with a resolving power between R=

λ / Δ λ

= 120 and 180. The spatial resolution of the images depends on the observation and is few hundreds of meters at the best. In this study, we retrieved the distribution of the photochemical haze (above 80 km) and the condensate mist layer (below 80 km) as a function of latitude, altitude, and tile throughout the Cassini era. We found a haze latitudinal distribution with an extinction increasing from the south to the north at the beginning of the Cassini mission. The distribution evolved around the North Spring Equinox and a turnover was completely achieved at the end of the Cassini mission. This evolution is linked to the stratospheric circulation that blows from the summer hemisphere to the winter polar region. The latitudinal distribution of the mist layer evolves differently than the haze distribution because it depends on both the circulation pattern in the low atmosphere and on the conditions of condensation for several species. The distribution of the mist layer is also modulated with the seasons, but always increases from the equator and inter-tropical latitude band to the poles.

These results yield a quantitative description of the aerosol layer on Titan and its seasonal evolution. This has been compared with previous works and with the output of the Titan Planetary Climate Model. Producing such results is quite important to constrain climate models. In return, we expect from these climate models to be helpful in fully understanding the meaning of our results and more generally in characterizing Titan’s climate.

从2004年到2017年，卡西尼号环绕土星的轨道飞行器用多种仪器监测了土卫六13年。这大约是土卫六年的一半，这段时间包括2009年北春分（NSE）的主要季节变化，可以观察到。卡西尼号上的视红外测绘光谱仪（VIMS）对土卫六进行了大量观测，通常以光谱图像的形式呈现。VIMS探测器红外部分的观测光谱范围为0.88 ~ 5.12μm，分辨能力为R= λ/Δλ = 120 ~ 180。图像的空间分辨率取决于观测，最好是几百米。在这项研究中，我们检索了整个卡西尼时代光化学雾（80公里以上）和冷凝雾层（80公里以下）作为纬度、海拔和瓦的函数的分布。我们发现，在卡西尼号任务开始时，雾霾的纬度分布从南到北逐渐消失。这种分布在北春分附近演变，在卡西尼号任务结束时完全实现了一次更替。这种演变与从夏季半球吹向冬季极地的平流层环流有关。雾层的纬向分布与霾分布的演变不同，因为雾层的纬向分布既取决于低层大气的环流型态，也取决于几种类型的凝结条件。雾层的分布也随季节变化而变化，但从赤道和热带纬带到两极总是增加的。这些结果对土卫六上的气雾层及其季节演变进行了定量描述。这已经与以前的工作和泰坦行星气候模型的输出进行了比较。产生这样的结果对于约束气候模型非常重要。作为回报，我们期望这些气候模型有助于充分理解我们的结果的意义，并更广泛地描述土卫六的气候特征。

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引用次数: 0

Dynamical evolution of the Uranian satellite system III. The passage through the 7/4 MMR between Miranda and Ariel 天王星卫星系统的动态演化3。米兰达和爱丽儿之间的7/4 MMR通道

IF 3 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2026-05-15 Epub Date: 2026-01-27 DOI: 10.1016/j.icarus.2026.116974

Sérgio R.A. Gomes, Tibi Keizer

The passage through the

5 / 3

mean-motion resonance between Ariel and Umbriel, two of Uranus’s largest moons, still raises several open questions. Previous studies suggest that, in order to reproduce the current orbital configuration, Ariel must have had an eccentricity of approximately ∼0.01 before the resonance encounter, which would prevent resonant capture. However, the rapid tidal circularization of Ariel’s orbit implies that some prior mechanism must have excited its eccentricity before the resonance encounter. In this work, we performed a large number of simulations using an

N

-body integrator to assess whether the earlier

7 / 4

mean-motion resonance between Miranda and Ariel could serve as a mechanism to increase Ariel’s eccentricity. Our results show that, due to divergent migration, resonance capture does not occur. As the satellites cross the nominal resonance, Ariel’s eccentricity is only excited to

3.4 \times 1 0^{- 4}

, substantially smaller than the required value. Therefore, the

7 / 4

mean-motion resonance is not a viable mechanism for increasing Ariel’s eccentricity.

天王星两颗最大的卫星Ariel和Umbriel之间的5/3平均运动共振，仍然引发了几个悬而未决的问题。先前的研究表明，为了重现当前的轨道结构，Ariel在共振相遇之前必须具有大约0.01的离心率，这将阻止共振捕获。然而，Ariel轨道的快速潮汐圆化意味着在共振相遇之前一定有某种先前的机制激发了它的偏心。在这项工作中，我们使用n体积分器进行了大量模拟，以评估Miranda和Ariel之间早期的7/4平均运动共振是否可以作为增加Ariel偏心的机制。我们的结果表明，由于发散性迁移，共振捕获不会发生。当卫星越过名义共振时，Ariel的偏心率仅被激发到3.4×10−4，大大小于所需值。因此，7/4平均运动共振不是增加Ariel偏心的可行机制。

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引用次数: 0

Topological analysis of Europa’s fracture networks 木卫二裂缝网络的拓扑分析

IF 3 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2026-05-01 Epub Date: 2026-01-12 DOI: 10.1016/j.icarus.2026.116943

V.F. Peixoto , B.E. Morgado , F.M.W. Tognoli , C. Haslebacher

Europa’s surface is dominated by lineaments that record its tectonic evolution and provide key constraints on ice-shell dynamics. While previous studies have primarily relied on descriptive mapping, here we apply a quantitative framework integrating geometric and topological analyses to characterize fracture networks within high-resolution Galileo SSI mosaics. Lineaments were mapped using the deep learning tool LineaMapper followed by manual refinements in QGIS, producing a consistent dataset across two representative areas located in the leading and trailing hemispheres. From these networks, we computed spacing, density (

P_{21}

), and orientation, and performed a topological analysis with the Python package Fractopo. Within the specific areas investigated, the trailing-hemisphere area exhibits higher lineament density, greater node frequency, and more segmented networks, whereas the leading-hemisphere area contains longer, more continuous lineaments with lower connectivity. Orientation patterns further show that longer fractures preferentially align E–W, consistent with tidal stress predictions. These results indicate that fracture networks in the examined sectors are moderately connected and spatially heterogeneous, reflecting local variations in stress and terrain type. The integrated approach presented here provides a quantitative baseline for future studies and will be particularly valuable for interpreting the unprecedented spatial coverage and resolution expected from ESA’s JUICE and NASA’s Europa Clipper missions.

木卫二的表面主要由记录其构造演化并提供冰壳动力学关键约束的线条组成。虽然以前的研究主要依赖于描述性映射，但在这里，我们应用了一个定量框架，结合几何和拓扑分析来表征高分辨率Galileo SSI马赛克中的裂缝网络。使用深度学习工具LineaMapper绘制线条，然后在QGIS中进行手动细化，在位于前半球和后半球的两个代表性区域生成一致的数据集。从这些网络中，我们计算了间距、密度（P21）和方向，并使用Python包Fractopo进行了拓扑分析。在研究的特定区域中，后半球区域具有更高的线状密度、更高的节点频率和更多的分段网络，而前半球区域包含更长、更连续的线状结构，连通性较低。定向模式进一步表明，较长的裂缝优先沿东西向排列，与潮汐应力预测一致。研究结果表明，裂缝网络具有中等连通性和空间异质性，反映了应力和地形类型的局部变化。这里提出的综合方法为未来的研究提供了定量基线，对于解释ESA JUICE和NASA的木卫二快船任务所期望的前所未有的空间覆盖和分辨率尤其有价值。

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引用次数: 0

On the forced orbital plane of the Hilda asteroids 在希尔达小行星的强制轨道平面上

IF 3 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2026-05-01 Epub Date: 2026-01-17 DOI: 10.1016/j.icarus.2026.116959

Ian C. Matheson , Renu Malhotra

Hilda-group asteroids librate in Jupiter’s interior 3:2 mean motion resonance. We estimate that the Hilda group is observationally complete up to absolute magnitude

H \leq 16.3

. This provides a statistically useful sample of thousands of resonant objects, all within a narrow range of semi-major axes, to compare with theoretical expectations of their orbital distribution from dynamical theory. We use von Mises–Fisher statistics to calculate the sample mean planes and mean plane uncertainties for the Hilda group and its Hilda, Schubart, and Potomac collisional subfamilies. Although Laplace–Lagrange linear secular theory is considered inapplicable within mean motion resonances, we find that the Laplace plane and the orbital plane of Jupiter are both statistically indistinguishable from the sample mean plane of the Hildas. In future work, we intend to extend this investigation to resonant populations in the Kuiper belt so as to further test the validity of Laplace–Lagrange linear secular theory for the mean planes of resonant populations.

希尔达群小行星在木星内部的平均运动共振为3:2。我们估计希尔达星群在绝对星等H≤16.3的范围内是观测完备的。这为数千个共振物体提供了一个统计上有用的样本，它们都在半长轴的狭窄范围内，可以与动力学理论对它们轨道分布的理论期望进行比较。我们使用von Mises-Fisher统计来计算Hilda群及其Hilda、Schubart和Potomac碰撞亚族的样本平均平面和平均平面不确定性。虽然拉普拉斯-拉格朗日线性长期理论被认为不适用于平均运动共振，但我们发现木星的拉普拉斯平面和轨道平面与希尔达斯的样本平均平面在统计上无法区分。在未来的工作中，我们打算将这项研究扩展到柯伊伯带的共振种群，以进一步验证共振种群平均平面的拉普拉斯-拉格朗日线性长期理论的有效性。

引用次数: 0

Terahertz characteristics of regolith simulants: Effects of bulk density and water content on electromagnetic response for planetary remote sensing 模拟风化层的太赫兹特性：体积密度和含水量对行星遥感电磁响应的影响

IF 3 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2026-05-01 Epub Date: 2025-12-10 DOI: 10.1016/j.icarus.2025.116911

Suyun Wang, Kazuma Hiramatsu

Electromagnetic properties of regolith are critical for understanding planetary subsurface structure and resource potential. However, their behavior in the terahertz (THz) frequency range remains poorly characterized. THz waves are particularly sensitive to fine-grained structure and hydration state, offering new opportunities for high-resolution planetary subsurface sensing. To investigate these interactions, we performed THz reflection measurements on FJS-1 lunar regolith simulants while varying bulk density (1.44–1.81 g/cm

^{3}

) and volumetric water content (0–46.1%). Measurements were conducted across 220–500 GHz using dual polarizations (HH, VV) and angle-resolved configurations (20–70° incidence angles). Results show clear density and hydration dependence of THz reflection coefficients, with Brewster angle shifts indicating changes in dielectric contrast. VV polarization demonstrated significantly higher sensitivity to both variables than HH polarization, enabling improved discrimination of subsurface properties. Results provide new experimental constraints on THz wave propagation in granular materials under controlled conditions, establishing a measurement framework applicable to future planetary remote sensing strategies for landing site assessment and water detection.

风化层的电磁特性是了解行星地下结构和资源潜力的关键。然而，它们在太赫兹（THz）频率范围内的行为特征仍然很差。太赫兹波对细粒结构和水合状态特别敏感，为高分辨率行星地下传感提供了新的机会。为了研究这些相互作用，我们在FJS-1模拟月球风化层上进行了太赫兹反射测量，同时改变了堆积密度（1.44-1.81 g/cm3）和体积含水量（0-46.1%）。测量在220-500 GHz范围内进行，使用双偏振（HH， VV）和角度分辨配置（20-70°入射角）。结果表明，太赫兹反射系数与密度和水化关系明显，布鲁斯特角的变化表明介电对比度的变化。VV偏振对这两个变量的敏感性明显高于HH偏振，从而提高了对地下性质的识别。研究结果提供了受控条件下颗粒状材料中太赫兹波传播的新实验约束，建立了适用于未来行星遥感着陆点评估和水探测策略的测量框架。

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引用次数: 0

Mastcam-Z analog spectral imager (MASI): A Mastcam-Z testbed and field instrument Mastcam-Z模拟光谱成像仪（MASI）：一种Mastcam-Z测试平台和现场仪器

IF 3 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2026-05-01 Epub Date: 2026-01-13 DOI: 10.1016/j.icarus.2026.116948

M.N. Barrington , C.D. Tate , A.G. Hayes

Mastcam-Z is a stereoscopic, zoomable multispectral imaging system located on the Remote Sensing Mast (RSM) of the Perseverance Rover. Mastcam-Z is the first zoomable multispectral imaging system flown on a NASA spacecraft. The Mastcam-Z Analog Spectral Imager is a Mastcam-Z emulator built at Cornell University for three primary purposes: 1) to serve as a testbed for the pre-flight radiometric and geometric calibration of Mastcam-Z, 2) to characterize Mastcam-Z anomalies observed during calibration and operation, and 3) to act as a field instrument for collecting terrestrial analog multispectral data with the same resolution and spectral characteristics as Mastcam-Z images. MASI is engineered using a combination of commercial off-the-shelf (COTS) components and Mastcam-Z flight spare hardware and is calibrated using a similar set of algorithms to Mastcam-Z. Herein, we show that MASI produces reflectance values that are similar to Mastcam-Z laboratory and inflight values, and provide a detailed description of MASI's hardware, software, and spectral data products.

Mastcam-Z是一种立体、可缩放的多光谱成像系统，安装在毅力号火星车的遥感桅杆（RSM）上。Mastcam-Z是第一个在NASA航天器上飞行的可变焦多光谱成像系统。Mastcam-Z模拟光谱成像仪是由康奈尔大学建造的Mastcam-Z模拟器，主要有三个目的：1)作为Mastcam-Z飞行前辐射和几何校准的测试平台，2)表征校准和操作过程中观察到的Mastcam-Z异常，3)作为收集地面模拟多光谱数据的现场仪器，具有与Mastcam-Z图像相同的分辨率和光谱特性。MASI的设计结合了商用现货（COTS）组件和Mastcam-Z飞行备用硬件，并使用与Mastcam-Z类似的一套算法进行校准。在这里，我们展示了MASI产生的反射率值与Mastcam-Z实验室和飞行值相似，并提供了MASI硬件，软件和光谱数据产品的详细描述。

引用次数: 0

Alkali recondensation into chondrules 碱缩聚成球粒

IF 3 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2026-05-01 Epub Date: 2026-01-23 DOI: 10.1016/j.icarus.2026.116970

Emmanuel Jacquet , Yves Marrocchi , Sébastien Charnoz

While sub-mm melt droplets should rapidly lose alkali elements in a vacuum at liquidus temperatures, chondrules are only modestly depleted in them (by less than one order of magnitude). The detection of sodium in olivine cores has previously suggested very high saturating partial pressures of gaseous sodium, but we show that alkalis were lost during heating and recondensed at lower temperatures, essentially in the present-day chondrule mesostases. This recondensation was accompanied by mass-dependent enrichment in light isotopes (for multi-isotope alkalis such as K and Rb), but its limited extent indicates a cooling acceleration (or “quenching”). The isotopic fractionation also constrains the ratio of the chondrule density and the cooling rate prior to the quench around

1 0^{- 6}

kg.m

^{- 3}

.K

^{- 1}

.h suggesting densities above

\sim

10

^{- 6}

kg/m

^{3}

. In a nebular context, this is achievable by radial and vertical concentrations near pressure bumps.

当小于毫米的熔融液滴在液态温度下的真空中会迅速失去碱元素时，球粒在其中只会适度地消耗（少于一个数量级）。在橄榄石岩心中检测到的钠先前表明，气态钠的饱和分压非常高，但我们表明，碱在加热过程中丢失，并在较低温度下重新凝聚，主要是在今天的球粒中间瘤中。这种重凝聚伴随着轻同位素（如K和Rb等多同位素碱）的质量依赖富集，但其有限程度表明冷却加速（或“淬火”）。同位素分馏还限制了球粒密度与淬火前冷却速率的比值约为10−6 kg.m−3.K−1.h，表明球粒密度高于~ 10−6 kg/m3。在星云环境中，这可以通过靠近压力凸起的径向和垂直浓度来实现。

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引用次数: 0

Inferring meteoroid properties with dynamic nested sampling: A case study of orionid and capricornid shower meteors 用动态嵌套抽样推断流星体的性质：以猎户座和摩羯座流星雨为例

IF 3 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2026-05-01 Epub Date: 2026-01-23 DOI: 10.1016/j.icarus.2026.116963

Maximilian Vovk , Peter G. Brown , Denis Vida , Daeyoung Lee , Emma G. Harmos

<div><h3>Importance:</h3><div>Accurate estimation of meteoroid bulk density is crucial for assessing spacecraft impact hazards of sub-millimeter to millimeter-sized meteoroids, which represent the bulk of the hazard.</div></div><div><h3>Research Gap:</h3><div>Previous studies utilized manual or optimization methods for fitting numerical meteoroid ablation and fragmentation models to optical meteor observations. However, these methods struggled with reliably estimating meteoroid physical properties and the associated uncertainties due to the subjectivity of the modeling approach.</div></div><div><h3>Objective:</h3><div>We aim to develop a global and statistically robust optimization method for inferring the physical properties of individual meteors, focusing on bulk density and fragmentation behavior, using multi-instrument optical data.</div></div><div><h3>Methodology:</h3><div>We apply Dynamic Nested Sampling to fit an erosion-fragmentation model to measurements of meteor light curve and deceleration. The method was applied to 15 shower meteors observed by the Canadian Automated Meteor Observatory’s (CAMO) mirror tracking and Electron-Multiplied Charge Coupled Device (EMCCD) systems. The method yields posterior distributions and Bayesian evidences for single and double fragmentations.</div></div><div><h3>Key Findings:</h3><div>Validation against four synthetic test cases demonstrated accurate recovery of known inputs, with best-guess solutions matching true parameters. We applied this method to 9 Orionids (ORI) and 6 <span><math><mi>α</mi></math></span> Capricornids (CAP) ranging in mass from <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>6</mn></mrow></msup></mrow></math></span> to <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>5</mn></mrow></msup></mrow></math></span> kg. The median bulk density was measured as <span><math><mrow><mn>15</mn><msubsup><mrow><mn>9</mn></mrow><mrow><mo>−</mo><mn>57</mn></mrow><mrow><mo>+</mo><mn>558</mn></mrow></msubsup></mrow></math></span> kg/m<span><math><msup><mrow></mrow><mrow><mn>3</mn></mrow></msup></math></span> for Orionid meteors and <span><math><mrow><mn>33</mn><msubsup><mrow><mn>3</mn></mrow><mrow><mo>−</mo><mn>114</mn></mrow><mrow><mo>+</mo><mn>1089</mn></mrow></msubsup></mrow></math></span> kg/m<span><math><msup><mrow></mrow><mrow><mn>3</mn></mrow></msup></math></span> for Capricornid meteors. These results are consistent with earlier studies: Orionids exhibit characteristics expected for meteoroids of cometary origin, whereas <span><math><mi>α</mi></math></span> Capricornids show systematically higher bulk densities. The CAP results show a second cluster around 1300 kg/m<span><math><msup><mrow></mrow><mrow><mn>3</mn></mrow></msup></math></span>, more inline with higher density asteroidal material, but our method achieves this using a more consistent and statistically robust estimation of uncertainties.</div></div><div><h3>Implications:</h3><

重要性：准确估计流星体的体积密度对于评估亚毫米到毫米大小的流星体的航天器撞击危害至关重要，它们代表了危害的大部分。研究空白：以往的研究采用人工或优化方法拟合流星光学观测的流星体烧蚀和碎片化数值模型。然而，由于建模方法的主观性，这些方法难以可靠地估计流星体的物理性质和相关的不确定性。目的：我们的目标是开发一种全球和统计稳健的优化方法来推断单个流星的物理性质，重点是体积密度和碎片行为，使用多仪器光学数据。方法：采用动态嵌套采样方法拟合侵蚀破碎模型，对流星光曲线和减速进行测量。该方法应用于加拿大自动流星观测站（CAMO）的镜面跟踪和电子倍增电荷耦合器件（EMCCD）系统观测到的15颗流星雨。该方法可以得到单次和双次碎片的后验分布和贝叶斯证据。主要发现：针对四个合成测试用例的验证演示了已知输入的准确恢复，以及与真实参数匹配的最佳猜测解决方案。我们将这种方法应用于9个猎户座（ORI）和6个α摩羯座（CAP），质量在10−6 ~ 10−5 kg之间。猎户座流星的中位体积密度为159−57+558 kg/m3，摩羯座流星为333−114+1089 kg/m3。这些结果与早期的研究是一致的：猎户座流星表现出彗星起源的流星体的特征，而α摩羯座流星则表现出更高的体积密度。CAP结果显示第二个星团约为1300 kg/m3，更符合高密度的小行星物质，但我们的方法使用更一致和统计上可靠的不确定性估计来实现这一目标。意义：开发的框架能够实现流星体物理特性的自动化，统计严格的表征。该方法将应用于更多的流星雨和零星流星，以表征跨轨道类物体的材料特性。

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引用次数: 0

Limit cycles and the climate history of Mars 极限循环和火星的气候历史

IF 3 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2026-05-01 Epub Date: 2026-01-14 DOI: 10.1016/j.icarus.2026.116945

Jacob Haqq-Misra

Evidence for fluvial features and standing liquid water indicate that Mars was a warmer and wetter place in its past; however, climate models have historically been unable to produce conditions to yield a warm early Mars under the faint young sun. Some models invoke thick greenhouse atmospheres to produce continuously warm conditions, but others have argued that available geologic evidence is more consistent with short-duration and transient warming events on an otherwise cold Mars. One possibility of harmonizing these perspectives is that early Mars experienced climate limit cycles that caused the climate to oscillate between short periods of warmth and prolonged periods of glaciation, due to modulation of greenhouse warming by the carbonate-silicate cycle. This study suggests that episodic limit cycling during the Noachian and Hesperian periods provides a hypothetical explanation for the timing and formation of fluvial features on Mars. A schematic time-forward trajectory of the full history of Mars is calculated using an energy balance climate model, which includes an active carbonate-silicate cycle, instellation changes due to the sun’s main sequence evolution, variations in the obliquity of Mars, and supplemental warming from additional greenhouse gases beyond carbon dioxide alone. These calculations demonstrate the viability of a climate history for Mars involving episodic limit cycling to enable the formation of the valley networks at 4.1-3.5 Ga and delta features at 3.3-3.0 Ga, interspersed with cold stable climates and ending in the late Amazonian in a carbon dioxide condensation regime. This schematic climate trajectory provides a plausible narrative that remains consistent with available geologic data, and further exploration of warming mechanisms for the climate of Mars should consider the possibility of episodic transient events driven by carbonate-silicate limit cycling.

河流特征和液态水的证据表明，火星过去是一个温暖潮湿的地方；然而，从历史上看，气候模型无法在微弱的年轻太阳下产生一个温暖的早期火星。一些模型援引厚厚的温室大气来产生持续的温暖条件，但另一些模型则认为，现有的地质证据更符合在寒冷的火星上发生的短时间和短暂的变暖事件。协调这些观点的一种可能性是，早期火星经历了气候极限循环，由于碳酸盐-硅酸盐循环对温室变暖的调节，导致气候在短时间的温暖期和长时间的冰期之间波动。这项研究表明，诺亚纪和希斯纪时期的幕式极限循环为火星上河流特征的时间和形成提供了一个假设性的解释。利用能量平衡气候模型计算了火星整个历史的时间向前轨迹示意图，其中包括活跃的碳酸盐-硅酸盐循环、太阳主序演化引起的安装变化、火星倾角的变化以及二氧化碳以外的额外温室气体的补充变暖。这些计算证明了火星气候历史的可行性，包括偶发性极限循环，使山谷网络在4.1-3.5 Ga形成，三角洲特征在3.3-3.0 Ga形成，点缀着寒冷稳定的气候，并在二氧化碳凝结状态下结束于亚马逊河晚期。这一气候轨迹示意图提供了一个与现有地质数据保持一致的合理叙述，并且对火星气候变暖机制的进一步探索应该考虑由碳酸盐-硅酸盐极限循环驱动的偶发性瞬变事件的可能性。

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引用次数: 0

Detecting and measuring Transverse Aeolian Ridges on Mars using deep learning 利用深度学习技术探测和测量火星上的横向风成脊

IF 3 2区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Icarus

Pub Date : 2026-05-01 Epub Date: 2026-01-13 DOI: 10.1016/j.icarus.2026.116947

Alexander M. Barrett , Matthew R. Balme , Elena A. Favaro , Mark J. Woods , Mateusz Malinowski , Laila Elsarky , Kylash Rajendran , James A. Holmes , Manish R. Patel

In this investigation, a Deep Learning (DL) approach was applied to measure the morphometry of Transverse Aeolian Ridges (TARs) on the surface of Mars. A large sample of TARs was segmented from High Resolution Imaging Science Experiment (HiRISE) images, the highest resolution remote sensing dataset presently available for the planet. HiRISE images located between 50°N and 50°S, and from all longitudes were selected. Morphometric parameters such as area, elongation, and orientation were retrieved for this sample using a supervised instance segmentation and geospatial analysis pipeline. The result is the most extensive catalogue of TAR morphometry to date extracted from ∼14 million candidate TARs in ∼7000 HiRISE Images. This was accomplished by training off-the-shelf DL models within a Geographic Information System (GIS) environment. A significant TAR population was found in approximately half of the images surveyed. TAR area, and the lengths of the long and short axes, were found to exhibit a positively skewed log-normal distribution; the median short axis length is 5 m, while the median long axis is 24 m. Median elongation is 0.24. Global TAR orientations are varied, although North-South oriented TARs are the most populous group. This is likely due to the strong east blowing winds predicted by GCM simulations of the modern martian climate. Here we present our latest results and use TAR orientation statistics to describe the emerging picture of global wind patterns on Mars during TAR forming epochs.

在这项研究中，深度学习（DL）方法被应用于测量火星表面横向风成脊（TARs）的形态。从高分辨率成像科学实验（HiRISE）图像中分割出大量的卫星样本，这是目前地球上可用的最高分辨率遥感数据集。HiRISE图像位于50°N和50°S之间，来自所有经度。使用监督实例分割和地理空间分析管道检索该样本的形态测量参数，如面积、伸长率和方向。结果是从~ 7000张HiRISE图像中的~ 1400万候选TAR中提取出迄今为止最广泛的TAR形态测量目录。这是通过在地理信息系统（GIS）环境中训练现成的深度学习模型来完成的。在大约一半的调查图像中发现了大量的西藏自治区人口。西藏自治区面积、长轴和短轴长度呈正斜对数正态分布；短轴长度中位数为5 m，长轴长度中位数为24 m。中位延伸率为0.24。虽然面向南北的TAR是人口最多的群体，但全球TAR的方向各不相同。这可能是由于GCM模拟现代火星气候预测的强劲的东风所致。在这里，我们展示了我们的最新结果，并使用TAR方向统计来描述在TAR形成时期火星上全球风模式的新图景。

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引用次数: 0

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