地球与行星天体物理学

• 新提交
• 交叉列表
• 替换

查看 最近的 文章

显示 2025年07月08日， 星期二 新的列表

新提交 (展示 25 之 25 条目 )

[1] arXiv:2507.03247 [中文pdf, pdf, html, 其他]

标题： 爆发彗星12P/庞斯-布鲁克斯的光学和近红外光谱 显示英文标题

标题： Optical and Near-Infrared Spectroscopy of the Outbursting Comet 12P/Pons-Brooks

Ruining Zhao, Bin Yang, Michael S. P. Kelley, Silvia Protopapa, Aigen Li, Yang Huang, Jifeng Liu

评论： 18页，4图，1表，已接受发表于ApJ

主题： 地球与行星天体物理学 (astro-ph.EP)

我们提供了对爆发的哈雷型彗星12P/Pons-Brooks的光学和近红外（NIR）观测。在2023年10月和11月的两次爆发期间，分别使用3米红外望远镜设施和帕洛马200英寸望远镜获得了三组NIR光谱。NIR光谱在1.5和2.0$\mu$m处显示出吸收特征，与水冰的诊断吸收带一致，并叠加在红色尘埃散射连续谱上。我们发现，吸收带和红色连续谱可以通过140-170 K范围内的微米级晶体冰以及亚微米级的耐火颗粒（例如非晶碳）很好地解释。此外，在2023年11月的爆发期间，使用丽江2.4米望远镜获得了一组光学光谱，该光谱显示了气态CN、C$_3$、C$_2$和NH$_2$的发射带。 C$_3$/CN 和 C$_2$/CN 比值表明 12P/庞斯-布鲁克斯在 C$_3$丰度上是“典型”的，但在 C$_2$上有所贫化。 2023 年 11 月爆发的特定动能估计为$\sim8\times10^3$ J kg$^{-1}$，表明可能的触发机制与 332P/池谷-牟田和 17P/霍尔姆斯类似，即非晶态水冰的结晶化。 从尘埃和气体的总质量损失中得出的耐火物质与冰的比例为$\sim$1.7--3.2，与 67P/丘留莫夫-格拉西缅科和 1P/哈雷的低端估计一致。 这表明可能是核体演化程度较低，或者爆发区域相对于整个核体富含冰质物质。 显示英文摘要

We present optical and near-infrared (NIR) observations of the outbursting, Halley-type comet 12P/Pons-Brooks. Three NIR spectra were obtained during two outbursts in October and November 2023, with the 3-meter Infrared Telescope Facility and the Palomar 200-inch Telescope, respectively. The NIR spectra exhibited absorption features at 1.5 and 2.0 $\mu$m, consistent with the diagnostic absorption bands of water ice, superimposed on a red dust-scattering continuum. We find that the absorption bands and the red continuum can be well explained by micrometer-sized crystalline ice at 140--170 K, along with sub-micrometer-sized refractory grains (e.g., amorphous carbon). In addition, an optical spectrum was obtained with the Lijiang 2.4-meter Telescope during the November 2023 outburst, which exhibited the emission bands of gaseous CN, C$_3$, C$_2$ and NH$_2$. The C$_3$/CN and C$_2$/CN ratios suggest that 12P/Pons-Brooks was ''typical'' in C$_3$ abundance but somewhat depleted in C$_2$. The specific kinetic energy of the 2023 November outburst is estimated to be $\sim8\times10^3$ J kg$^{-1}$, suggesting a likely triggering mechanism similar to 332P/Ikeya--Murakami and 17P/Holmes, i.e., the crystallization of amorphous water ice. A refractory-to-ice ratio of $\sim$1.7--3.2 is derived from the total mass loss of dust and gas, aligning with the lower-end estimates for 67P/Churyumov-Gerasimenko and 1P/Halley. This suggests either a less evolved nucleus or an outburst region enriched in icy materials relative to the bulk nucleus.

[2] arXiv:2507.03370 [中文pdf, pdf, html, 其他]

标题： 围绕吸积原行星的温暖气泡中CO的恢复及其可观测性 显示英文标题

标题： Resurgence of CO in a warm bubble around accreting protoplanets and its observability

O. Chrenko, S. Casassus, R. O. Chametla

评论： 已被A&A接收

主题： 地球与行星天体物理学 (astro-ph.EP) ; 太阳与恒星天体物理学 (astro-ph.SR)

原行星盘的冷外区预计会包含一个以中层为中心的区域，在该区域中气相CO分子冻结，其总体丰度较低。 该层在CO旋转发射线的通道图中表现为一个空洞。 我们探讨了冻结层是否能将嵌入的吸积原行星的原行星环境暴露给观测。 为此，我们进行了三维辐射气体-尘埃流体动力学模拟，直接将消光和光学深度与亚$\mu$米和毫米级尘埃颗粒的再分布联系起来。 考虑了一个具有吸积光度$\sim$$10^{-3}\,L_{\odot}$ 的木星质量行星作为标准情况。 吸积加热在行星周围维持了一个温暖的气泡，局部增加了气相CO分子的丰度。 出射天空图像的辐射转移预测显示，气泡在通道图中成为一个明显的CO发射源，表现为位于“蜻蜓翅膀”之间的低强度光学厚斑点，这些“蜻蜓翅膀”追踪了前侧和后侧形成线的表面。 气泡的发射强度几乎与示踪同位素无关，表明只要其信号能够从扩展的盘发射中分离出来，就具有非常丰富的可观测化学性质。 这可以通过在行星引起的间隙中光学薄或弱热分层的同位素实现，例如C$^{18}$O。 对于这些同位素，气泡在减去从盘运动学推导出的轴向平均通道图后的合成ALMA观测中成为最亮的残留物，从而实现了形成原行星的新自动检测。 相比之下，马蹄形流动持续地从原行星环境中耗尽大尘埃颗粒，使得该环境在亚毫米连续谱中不可观测，这与ALMA检测的稀缺性一致。 显示英文摘要

The cold outer regions of protoplanetary disks are expected to contain a midplane-centered layer in which gas-phase CO molecules freeze-out and their overall abundance is low. The layer then manifests itself as a void in the channel maps of CO rotational emission lines. We explore whether the frozen-out layer can expose the circumplanetary environment of embedded accreting protoplanets to observations. To this end, we performed 3D radiative gas-dust hydrodynamic simulations, directly linking opacities and optical depths to the redistribution of sub-$\mu$m- and mm-sized dust grains. A Jupiter-mass planet with accretion luminosity $\sim$$10^{-3}\,L_{\odot}$ was considered as the nominal case. The accretion heating sustains a warm bubble around the planet, locally increasing the abundance of gas-phase CO molecules. Radiative transfer predictions of the emergent sky images show that the bubble becomes a conspicuous CO emission source in channel maps, appearing as a low-intensity optically thick spot located in-between the `dragonfly wings' that trace the foreside and backside line-forming surfaces. The emission intensity of the bubble is nearly independent of the tracing isotopologue, suggesting a very rich observable chemistry, as long as its signal can be deblended from the extended disk emission. This can be achieved with isotopologues that are optically thin or weakly thermally stratified across the planet-induced gap, such as C$^{18}$O. For those, the bubble stands out as the brightest residual in synthetic ALMA observations after subtraction of axially-averaged channel maps inferred from the disk kinematics, enabling new automatic detections of forming protoplanets. By contrast, the horseshoe flow steadily depletes large dust grains from the circumplanetary environment which becomes unobservable in the sub-mm continuum, in accordance with the scarcity of ALMA detections.

[3] arXiv:2507.03538 [中文pdf, pdf, html, 其他]

标题： 外核对流的热化学模型与非均匀核幔边界热通量 显示英文标题

标题： Thermochemical models of outer core convection with heterogeneous core-mantle boundary heat flux

Souvik Naskar, Jonathan E. Mound, Christopher J. Davies, Andrew T. Clarke

评论： 提交至《地球与行星科学快报》

主题： 地球与行星天体物理学 (astro-ph.EP) ; 地球物理 (physics.geo-ph)

地核中的热化学对流由内核结晶释放潜热和轻元素所驱动。 核心动力学中的一个关键问题是，在地核-地幔边界下方是否存在一个稳定层。 最近的核对流模拟，考虑到CMB的不均匀性，提出了局部稳定区域（或区域反转透镜，RILs），而不是一个全球层，使得稳定和不稳定区域可以共存。 在本研究中，我们考虑了一系列针对Ekman数（$E=10^{-5}$）的热、化学和热化学对流模型，其热和化学通量雷诺数分别为$\widetilde{Ra}_T=30-4000$和$\widetilde{Ra}_C=30-100000$，热和化学普朗特数分别为$Pr_T=1$和$Pr_\xi=10$。 对纯化学模型的分析显示，在CMB下方出现了轻元素积累（LEA），根据化学强迫的强度，这会导致极地附近的局部稳定区域或全球层。 即使热场完全不稳定，这些化学分层区域在我们的热化学模型中仍然存在。 添加不均匀的CMB热通量会导致由热分层驱动的RILs形成。 这些热化学模型中的稳定区域的位置、性质和形态各不相同，这取决于热对流还是化学对流占主导地位。 在所研究的参数范围内，这些RILs厚度约为100公里，它们的强度和厚度通常随着热驱动强度的增加而增加；它们对化学驱动强度的敏感性相对较低。 我们的模拟揭示了地球地核顶部可能存在的多种稳定区域和/或全球层，其厚度和强度具有地震上合理的范围，也可能在地磁观测中留下特征。 显示英文摘要

Thermochemical convection in Earth's outer core is driven by the crystallisation of the inner core that releases latent heat and light elements. A key question in core dynamics is whether a stable layer exists just below the core-mantle boundary. Recent core convection simulations, accounting for CMB heterogeneities, propose locally stable regions (or regional inversion lenses, RILs) rather than a global layer, allowing both stable and unstable regions to coexist. In this study, we consider a suite of numerical simulations of thermal, chemical, and thermochemical convection models focussed on Ekman number ($E=10^{-5}$) with thermal and chemical flux Rayleigh numbers $\widetilde{Ra}_T=30-4000$ and $\widetilde{Ra}_C=30-100000$, and thermal and chemical Prandtl numbers $Pr_T=1$ and $Pr_\xi=10$. Analysis of purely chemical models reveals light element accumulation (LEA) below the CMB, resulting in either locally stable regions near the poles or global layers, depending on the strength of chemical forcing. These chemically stratified regions persist in our thermochemical models even if the thermal field is fully destabilising. The addition of a heterogeneous CMB heat flux leads to the formation of RILs driven by thermal stratification. Stable regions in these thermochemical models have varying locations, properties, and morphologies depending on whether thermal or chemical convection dominates. In the investigated parameter range, these RILs are O(100 km) thick, and their strength and thickness generally increase with the strength of thermal driving; they are comparatively less sensitive to the strength of chemical driving. Our simulations reveal a diverse range of possible stable regions and/or a global layer at the top of Earth's core, with a seismically plausible range of thickness and strength, which may also have a signature in geomagnetic observations.

[4] arXiv:2507.03562 [中文pdf, pdf, html, 其他]

标题： 行星质量极限VLT/SINFONI库：通过正向建模进行光谱提取和大气特征分析 显示英文标题

标题： The planetary-mass-limit VLT/SINFONI library: Spectral extraction and atmospheric characterization via forward modeling

P. Palma-Bifani, M. Bonnefoy, G. Chauvin, P. Rojo, P. Baudoz, B. Charnay, A. Denis, K. Hoch, S. Petrus, M. Ravet, A. Simonnin, A. Vigan

评论： 接受日期在《天文学与天体物理学》：2025年6月25日

主题： 地球与行星天体物理学 (astro-ph.EP) ; 太阳与恒星天体物理学 (astro-ph.SR)

我们旨在加深对行星质量伴星和孤立棕矮星的M-L转变的理解，并寻找这两个天体群体之间可能差异的证据。为此，我们展示了一组来自五个档案项目的21个VLT/SINFONI K波段观测数据，光谱分辨率为4000。我们的目标是测量大气特性，如温度、表面重力和金属丰度，以理解从M5到L5光谱类型的各种天体之间的相似性和差异性。我们使用TExTRIS代码提取了这些目标的光谱。随后，我们使用ForMoSA，一种用于光谱分析的贝叶斯正向建模工具，对它们进行建模，探索四类自洽的大气模型：ATMO、BT-Settl、Exo-REM和Sonora。在这里，我们展示了目标的光谱以及从大气建模中得出的参数。我们在M/L转变处观察到有效温度随光谱类型变化而下降超过500 K，这可能与当前大气模型的局限性有关。此外，我们报告了三个伴星（2M 0103 AB b、AB Pic b和CD-35 2722 b）的碳氧比测量结果，这些结果增加了已测量该值的系外行星列表。总之，VLT/SINFONI图书馆突出了两个关键点。首先，迫切需要进一步研究由自洽模型生成的光谱网格之间的差异，因为这些模型产生不同的结果，并未统一地探索参数空间。其次，我们没有在伴星和孤立棕矮星的K波段光谱中观察到明显的差异，这可能表明这些超级木星物体通过类似的过程形成；然而，这需要进一步研究。 显示英文摘要

We aim to deepen our understanding of the M-L transition on planetary-mass companions and isolated brown dwarfs, and search for evidence of possible differences between these two populations of objects. To this end, we present a set of 21 VLT/SINFONI K-band observations from five archival programs at a spectral resolution of 4000. We aim to measure atmospheric properties, such as temperature, surface gravity, and metallicity, to understand the similarities and differences between objects ranging from M5 to L5 in spectral type. We extracted the spectra of these targets with the TExTRIS code. Subsequently, we model them using ForMoSA, a Bayesian forward modeling tool for spectral analysis, exploring four families of self-consistent atmospheric models: ATMO, BT-Settl, Exo-REM, and Sonora. Here we present the spectra of our targets and the derived parameters from the atmospheric modeling. We observed a drop in effective temperature of more than 500 K as a function of spectral type at the M/L transition, likely related to limitations in the current atmospheric models. In addition, we report carbon-to-oxygen ratio measurements for three companions (2M 0103 AB b, AB Pic b, and CD-35 2722 b), which contribute to the growing list of exoplanets for which this value has been measured. In conclusion, the VLT/SINFONI Library highlights two key points. First, there is a critical need to further investigate the discrepancies among grids of spectra generated by self-consistent models, as these models yield varying results and do not uniformly explore the parameter space. Second, we do not observe apparent discrepancies in the K-band spectra between companions and isolated brown dwarfs, which potentially suggests that these super-Jupiter objects formed through a similar process; however, this warrants further investigation.

[5] arXiv:2507.03643 [中文pdf, pdf, html, 其他]

标题： 关于尘卷风直径、出现率和活动性 显示英文标题

标题： On Dust Devil Diameters, Occurrence Rates, and Activity

Brian Jackson, Lori Fenton, Ralph Lorenz, Chelle Szurgot, Joshua Gambill, Gwendolyn Arzaga

评论： 15页，5图，已被PSJ接收

主题： 地球与行星天体物理学 (astro-ph.EP)

作为一种在地球和火星上都会出现的现象，尘卷风的直径有助于确定两者向大气中注入的灰尘量——对于给定的尘埃通量密度（单位面积单位时间提升的灰尘），更宽的尘卷风会将更多的灰尘带入空气中。 然而，决定尘卷风直径的因素$D$以及它可能与周围环境条件的关系仍然不清楚。 此外，估算具有不同直径的尘卷风群体对大气尘埃预算的贡献需要对微分直径分布进行准确评估，但仍有大量工作尚未揭示最佳表示方式或解释其物理基础。 在本研究中，我们提出该分布遵循幂律 $\propto D^{-5/3}$，并提供了一个简单的物理解释来说明为什么该分布呈现这种形式。 通过拟合几项研究中报告的火星尘卷风直径分布，我们表明来自几项研究的数据支持这一提出的形态。 利用一个将尘卷风视为热力学热机的先前模型，我们还表明尘卷风的面积密度（单位面积的数量）$N_0$与它们的热力学效率 $\eta$和感热通量 $F_{\rm s}$的乘积成比例，如 $N_0 \propto \eta F_{\rm s}$所示。 显示英文摘要

As a phenomenon that occurs on Earth and on Mars, the diameter of a dust devil helps determine the amount of dust the devil injects into the atmosphere for both worlds -- for a given dust flux density (dust lifted per area per time), a wider devil will lift more dust into the air. However, the factors that determine a dust devil's diameter $D$ and how it might relate to ambient conditions have remained unclear. Moreover, estimating the contribution to an atmospheric dust budget from a population of dust devils with a range of diameters requires an accurate assessment of the differential diameter distribution, but considerable work has yet to reveal the best representation or explain its physical basis. In this study, we propose that this distribution follows a power-law $\propto D^{-5/3}$ and provide a simple physical explanation for why the distribution takes this form. By fitting diameter distributions of martian dust devil diameters reported in several studies, we show that the data from several studies support this proposed form. Using a previous model that treats dust devils as thermodynamic heat engines, we also show that the areal density of dust devils (number per unit area) $N_0$ scales with the product of their thermodynamic efficiency $\eta$ and the sensible heat flux $F_{\rm s}$ as $N_0 \propto \eta F_{\rm s}$.

[6] arXiv:2507.03696 [中文pdf, pdf, 其他]

标题： 与天王星处于外共振的小行星 显示英文标题

标题： A minor planet in an outer resonance with Uranus

Daniel Bamberger, K Ly, Sam Deen, Elvis Oliveira Mendes

评论： 5页，1图

主题： 地球与行星天体物理学 (astro-ph.EP)

我们找到了对半人马小行星2015 OU$_{194}$在2017和2018年的档案观测数据，这些数据将其数据弧长度从1.0年扩展到了3.5年。我们表明它处于海王星的外侧$3:4$均值运动共振中，此后称为U$_{3/4}$。该共振至少在过去的1000千年到未来的500千年内都是稳定的。我们在文献中没有发现有关该共振中已知天体的记载，或在海王星和冥王星轨道之间的任何其他共振中的天体。寻找其他候选天体时，我们发现2013 RG$_{98}$在当前时代附近几百年内也停留在U$_{3/4}$中。第三个候选天体2014 NX$_{65}$受到海王星的强烈影响。 显示英文摘要

We have located archival observations of the centaur 2015 OU$_{194}$ from 2017 and 2018, which extend its data-arc length from 1.0 to 3.5 years. We show that it is in an outer $3:4$ mean motion resonance with Uranus, henceforth referred to as U$_{3/4}$. The resonance is stable from at least 1000 kyrs in the past till 500 kyrs in the future. We find no mention in the literature of known objects in this resonance, or in any other resonance between the orbits of Uranus and Neptune. Looking for additional candidates, we find that 2013 RG$_{98}$ also stays in U$_{3/4}$ for several hundred kyrs around the present epoch. A third candidate, 2014 NX$_{65}$, is strongly influenced by Neptune.

[7] arXiv:2507.03716 [中文pdf, pdf, html, 其他]

标题： 边缘盘研究（EODS）II：飞碟盘的热结构 显示英文标题

标题： Edge-On Disk Study (EODS) II: Thermal Structure of the Flying Saucer Disk

S. Guilloteau (1), O. Denis-Alpizar (2), A. Dutrey (1), C. Foucher (1), S. Gavino (3), D. Semenov (4,5), V. Piétu (6), E. Chapillon (1,6), L. Testi (3), E. Dartois (7), E. di Folco (1), K. Furuya (8), U. Gorti (9), N. Grosso (10), Th. Henning (4), J.M. Huré (1), A. Kospal (11), F. LePetit (12), L. Majumdar (13), H. Nomura (14), N.T. Phuong (15), M. Ruaud (9), Y.W. Tang (16), S. Wolf (17) ((1) Univ. Bordeaux, CNRS, Laboratoire d'Astrophysique de Bordeaux (LAB), UMR 5804, F-33600 Pessac, France (2) Departamento de Física, Facultad de Ciencias, Universidad de Chile, Av. Las Palmeras 3425, Nuñoa, Santiago, Chile. (3) Dipartimento di Fisica e Astronomia "Augusto Righi", ALMA Mater Studiorum - Universiti. Bologna, via Gobetti 93/2, I-40190 Bologna, Italy (4) Max-Planck-Institut für Astronomie (MPIA), Königstuhl 17, D-69117 Heidelberg, Germany (5) Department of Chemistry, Ludwig-Maximilians-Universität, Butenandtstr. 5-13, D-81377 München, Germany (6) IRAM, 300 Rue de la Piscine, F-38406 Saint Martin d'Hères, France (7) Institut des Sciences Moléculaires d' (8) RIKEN Cluster for Pioneering Research, 2-1 Hirosawa, Wako-shi, Saitama 351-0198, Japan (9) Carl Sagan Center, SETI Institute, Mountain View, CA, USA (10) Aix-Marseille Univ, CNRS, CNES, LAM, Marseille, France Orsay, CNRS, Univ. Paris-Saclay, Orsay, France (11) Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Konkoly-Thege Miklós út 15-17, 1121 Budapest, Hungary (12) LUX, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, 92190 Meudon, France (13) Exoplanets and Planetary Formation Group, School of Earth and Planetary Sciences, National Institute of Science Education and Research, Jatni 752050, Odisha, India (14) National Astronomical Observatory of Japan, Division of Science, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Kanto Japan (15) Vietnam National Space Center, Vietnam Academy of Science and Technology, 18, Hoang Quoc Viet, Nghia Do, Cau Giay, Ha Noi, Vietnam (16) Academia Sinica Institute of Astronomy and Astrophysics, 11F of AS/NTU Astronomy-Mathematics Building, No.1, Sec.4, Roosevelt Rd, Taipei 106319, Taiwan, R.O.C (17) Institut für Theoretische Physik und Astrophysik, Christian-Albrechts-Universität zu Kiel, Leibnizstraße 15, 24118 Kiel, Germany)

评论： 10页，9图，将发表于《天文学与天体物理学》

主题： 地球与行星天体物理学 (astro-ph.EP) ; 太阳与恒星天体物理学 (astro-ph.SR)

上下文。原行星盘中的尘埃和气体温度在其化学演化中起着关键作用，并影响行星形成过程。 目标。我们尝试对飞行器盘边缘的尘埃和CO温度分布进行精确测量。 方法。我们利用了飞行器盘的独特性质，其边缘朝向的几何结构以及其在不同亮度温度的CO云前方的有利位置，以提供独立的尘埃温度约束。 我们将其与使用辐射转移代码DiskFit得出的尘埃温度和CO气体温度进行了比较。 结果。我们发现气体温度存在明显的垂直梯度，其中盘的中平面温度较低（10 K），而在CO层中，距离为100 au处的温度为27 K，随着指数0.3下降。 还发现了中平面以下约1个尺度高度处CO耗竭的直接证据。 在此高度，气体温度为15-20 K，与预期的CO冻结温度一致。 该尘埃盘在345 GHz处呈现光学薄，并表现出适度的沉降。 显示英文摘要

Context. The dust and gas temperature in proto-planetary disks play critical roles in determining their chemical evolution and influencing planet formation processes. Aims. We attempted an accurate measurement of the dust and CO temperature profile in the edge-on disk of the Flying Saucer. Methods. We used the unique properties of the Flying Saucer, its edge-on geometry and its fortunate position in front of CO clouds with different brightness temperatures to provide independent constraints on the dust temperature. We compared it with the dust temperature derived using the radiative transfer code DiskFit and the CO gas temperature. Results. We find clear evidence for a substantial gas temperature vertical gradient, with a cold (10 K) disk mid-plane and a warmer CO layer where T(r) is 27 K at 100 au, dropping with exponent 0.3. Direct evidence for CO depletion in the mid-plane, below about 1 scale height, is also found. At this height, the gas temperature is 15-20 K, consistent with the expected CO freeze out temperature. The dust disk appears optically thin at 345 GHz, and exhibits moderate settling.

[8] arXiv:2507.03741 [中文pdf, pdf, html, 其他]

标题： 评估在完整柯伊伯带形成模型中分离天体的胚胎起源 显示英文标题

标题： Evaluating an Embryo Origin for Detached TNOs within Full Kuiper Belt Formation Models

Nathan A. Kaib, Chadwick A. Trujillo, Scott S. Sheppard

评论： 12页，8图，已接受发表于《Icarus》

主题： 地球与行星天体物理学 (astro-ph.EP)

随着近日点位于海王星之外，但半长轴和偏心率表明受到显著扰动，分离的海王星外天体（TNOs）的起源仍然是一个动力学谜题。 特别是近日点倾角低于约25度的分离TNOs，目前在现代太阳系中任何已知机制都难以产生。 一个关于分离TNOs起源的显著假说是，在柯伊伯带形成过程中，一个~火星至地球质量的行星胚胎将这些天体的近日点从海王星那里分离出来，之后该胚胎本身被弹射出去。 我们通过模拟柯伊伯带从原始星子带形成的场景来数值建模这一情景，该原始星子带通过巨行星的迁移而分散。 除了约100,000个柯伊伯带天体外，我们的每个模拟都包含原始带中假设的胚胎种群。 我们发现，这些胚胎不太可能达到高近日点、大半长轴轨道，以有效地将TNO的近日点从海王星的影响中分离出来。 此外，胚胎通常需要至少1亿年才能到达这些不太可能的轨道，在此之前，大部分原始带已经被行星弹射出去，限制了可以被分离的可用种群数量。 最后，我们的胚胎所分离的TNOs始终具有更偏向小值的半长轴分布，这与观测到的分离TNOs不同。 因此，我们得出结论，原始柯伊伯带中的行星胚胎不太可能是分离TNOs起源的主要机制。 显示英文摘要

With perihelia well beyond Neptune, but semimajor axes and eccentricities indicative of substantial perturbation, the origins of detached trans-Neptunian objects (TNOs) remain a dynamical puzzle. In particular, detached TNOs with orbital inclinations below ~25 degrees are not easily generated from any known mechanism currently in the modern solar system. One notable hypothesis for the origins of detached TNOs is that a ~Mars- to Earth-mass planetary embryo detached the perihelia of these objects from Neptune during the process of Kuiper belt formation before the embryo itself was ejected. We numerically model this scenario via simulations of Kuiper belt formation from a primordial planetesimal belt that is dispersed through the migration of the giant planets. In addition to ~100,000 Kuiper belt objects, each of our simulations contains a hypothetical population of embryos in the primordial belt. We find that our embryos are unlikely to reach the high-perihelion, large semimajor axis orbit necessary to efficiently detach TNO perihelia from Neptune's influence. Moreover, embryos will typically take at least 100 Myrs to reach these unlikely orbits, at which point most of the primordial belt will have already been ejected by the planets, limiting the available population that can be detached. Finally, the TNOs that our embryos do detach consistently have a semimajor axis distribution that is more biased toward small values than observed detached TNOs have. Thus, we conclude that planetary embryos in the primordial Kuiper belt are not likely to have been the primary mechanism for the origin of detached TNOs.

[9] arXiv:2507.03760 [中文pdf, pdf, html, 其他]

标题： 天王星外天体颜色的原始性因果证据 显示英文标题

标题： Causal Evidence for the Primordiality of Colors in Trans-Neptunian Objects

Benjamin L. Davis, Mohamad Ali-Dib, Yujia Zheng, Zehao Jin, Kun Zhang, Andrea Valerio Macciò

评论： 被ML4Astro 2025（机器学习在天体物理学中的应用研讨会，ICML 2025）接受

主题： 地球与行星天体物理学 (astro-ph.EP) ; 机器学习 (cs.LG)

冥王星外天体（TNOs）颜色的起源是一个关键的未解问题，对于理解我们太阳系的历史至关重要。最近的观测调查揭示了TNOs的偏心率和倾角与其颜色之间的相关性。这重新引发了关于这些颜色是否反映了TNO形成时的条件还是其后续碰撞演化的长期争论。在本研究中，我们使用基于因果图的模型无关、数据驱动的方法，以98.7%的确定性解决了这个问题。首先，作为一项合理性检查，我们展示了我们的模型如何盲目的复制目前公认的TNO动力学历史，而无需任何轨道建模或基于物理的假设。事实上，我们的因果模型（对海王星的存在一无所知）预测了一个未知的扰动天体，即海王星。然后，我们展示了该模型如何以高确定性预测TNO的颜色是其倾角分布的根本原因，而不是相反。这强烈表明TNO的颜色反映了潜在的动力学特性，最可能是它们的形成位置。此外，我们的因果模型排除了由后续辐射引起显著颜色变化的形成情景。因此，我们得出结论，TNO的颜色主要是原始的。 显示英文摘要

The origins of the colors of Trans-Neptunian Objects (TNOs) represent a crucial unresolved question, central to understanding the history of our Solar System. Recent observational surveys have revealed correlations between the eccentricity and inclination of TNOs and their colors. This has rekindled the long-standing debate on whether these colors reflect the conditions of TNO formation or their subsequent collisional evolution. In this study, we address this question with 98.7% certainty, using a model-agnostic, data-driven approach based on causal graphs. First, as a sanity check, we demonstrate how our model can replicate the currently accepted paradigms of TNOs' dynamical history, blindly and without any orbital modeling or physics-based assumptions. In fact, our causal model (with no knowledge of the existence of Neptune) predicts the existence of an unknown perturbing body, i.e., Neptune. We then show how this model predicts, with high certainty, that the color of TNOs is the root cause of their inclination distribution, rather than the other way around. This strongly suggests that the colors of TNOs reflect an underlying dynamical property, most likely their formation location. Moreover, our causal model excludes formation scenarios that invoke substantial color modification by subsequent irradiation. We therefore conclude that the colors of TNOs are predominantly primordial.

[10] arXiv:2507.03819 [中文pdf, pdf, html, 其他]

标题： 使用HWO日冕仪的成像偏振测量检测外星宜居世界和光合作用生命 显示英文标题

标题： Detecting alien living worlds and photosynthetic life using imaging polarimetry with the HWO coronagraph

Svetlana Berdyugina, Lucas Patty, Jonathan Grone, Brice Demory, Kim Bott, Vincent Kofman, Giulia Roccetti, Kenneth Goodis Gordon, Frans Snik, Theodora Karalidi, Victor Trees, Daphne Stam, Mary N. Parenteau

评论： HWO科学案例

主题： 地球与行星天体物理学 (astro-ph.EP)

我们的地球是我们所知道的唯一的生命行星，它为我们提供了线索，表明光合作用生命形式可能在其他系外行星上存在数十亿年。 地表光合作用生命（PSLife）的光谱偏振特征在实验室中得到了很好的研究，并通过空间和航空仪器进行了遥感探测。 这些测量揭示了一个惊人的生物标志，即与生物色素（生物色素）的宽吸收带相关的极强线性偏振（百分之十几）。 此外，独特的圆偏振特征与生物色素和其他复杂大分子相关，作为手性纯度的标志，这是地表生命形式中普遍存在的现象。 因此，使用HWO日冕仪以前所未有的对比度直接成像的系外行星的低分辨率光谱或多波段偏振测量是一种发现系外生命的新机会。 在这里，我们提出进行两次调查和两次后续观测计划。 调查1将通过线偏振测量检测大气、云层和液态地表水（海洋）来确定潜在可居住的行星（PHPs）。 调查2将在PHPs中通过搜索与地球生物色素相似的强而宽的吸收带相关的强线性偏振特征来识别生命世界（LW）候选者。 后续计划3将获得LWs的多色表面图，确定具有外星生物色素（exoBPs）的外星光合作用生物的分布和丰度，并将其特性与大气和地表成分相关联。 后续计划4将使用圆偏振来验证exoBPs的手性纯度。 这种全面的方法旨在为最终的问题“我们在宇宙中是孤独的吗？”提供一个定量的答案。 显示英文摘要

Our Earth, being the only living planet that we know, provides us with clues that photosynthetic life-forms may be dominant on other exoplanets for billions of years. Spectropolarimetric signatures of the terrestrial photosynthetic life (PSLife) are well studied in the lab and remotely sensed with space and airborne instrumentation. An astonishing biosignature revealed by these measurements is an extremely strong linear polarization (tens \%) associated with broad absorption bands of biological pigments (biopigments) driving photosynthesis in various organisms. Also, unique circular-polarization signatures are associated with biopigments and other complex macromolecules as a sign of homochirality which is ubiquitous in terrestrial life forms. Thus, low-resolution spectro- or multi-band polarimetry of exoplanets directly imaged at an unprecedented contrast using the HWO coronagraph is a novel opportunity for a robust discovery of life on exoplanets. Here we propose to carry out two surveys and two follow-up observing programs. Survey 1 will identify potentially habitable planets (PHPs) through detection of atmospheres, clouds and liquid surface water (ocean) using linear polarimetry. Survey 2 will identify Living World (LW) candidates among PHPs by searching for strong linear polarization signatures associated with strong and broad absorption bands reminiscent of terrestrial biopigments. Follow-up program 3 will obtain multi-color surface maps of LWs, determine the distribution and abundance of alien photosynthetic organisms with exo-biopigments (exoBPs) and correlate their properties with the atmospheric and surface compositions. Follow-up program 4 will employ circular polarization to verify homochirality of exoBPs. This comprehensive approach aims at providing a quantitative answer to the ultimate question "Are we are alone in the Universe?".

[11] arXiv:2507.03850 [中文pdf, pdf, html, 其他]

标题： 海洋潮汐在围绕低质量恒星运行的异步自转行星上 显示英文标题

标题： Ocean Tides on Asynchronously Rotating Planets Orbiting Low-mass Stars

Jiaru Shi, Jun Yang, Dorian S. Abbot, Yonggang Liu, Wanying Kang, Yufeng Lin

主题： 地球与行星天体物理学 (astro-ph.EP)

行星在低质量恒星的液态水宜居带内会经历大的潮汐力，是地球上的$10^3$到$10^4$倍，这是由于宜居带与恒星之间的距离较小。 因此，这些行星上的固体内潮、海洋潮汐和大气潮汐可能比地球上的强得多，但很少有研究明确模拟海洋潮汐。 在这里，我们首次进行了全球海洋潮汐模拟，并表明自转不同步且偏心率较大的行星上的海洋潮汐高度可达$\mathcal{O}(1000)\,\mathrm{m}$，流速可达$\mathcal{O}(10)\,\mathrm{m\,s^{-1}}$。 潮汐与海底地形之间的相互作用可以引起大的能量耗散，平均而言为$\sim\mathcal{O}(100)\,\mathrm{W\,m^{-2}}$。 这种潮汐能量耗散可以通过1到2个数量级显著加速轨道演化。 然而，对于偏心率较小的行星，海洋潮汐要弱得多，但仍与现代地球相当。 我们的结果表明，围绕低质量恒星运行的偏心行星上的海洋潮汐比地球上的强大几个数量级，可以显著影响地表地理和轨道演化。 显示英文摘要

Planets in the liquid-water habitable zone of low-mass stars experience large tidal forces, $10^3$ to $10^4$ times those on Earth, due to the small distance between the habitable zone and the host stars. Therefore, interior solid tides, ocean tides and atmospheric tides on these planets could be much stronger than that on Earth, but rare work has been done to explicitly simulate the ocean tides. Here, for the first time, we perform global ocean tide simulations and show that ocean tides on asynchronously rotating planets with large eccentricities can reach $\mathcal{O}(1000)\,\mathrm{m}$ in height and $\mathcal{O}(10)\,\mathrm{m\,s^{-1}}$ in flow speed. Interactions between tide and bottom topography can induce large energy dissipation, $\sim\mathcal{O}(100)\,\mathrm{W\,m^{-2}}$ in global mean. This tidal energy dissipation can strongly accelerate orbital evolution by 1-2 orders of magnitude. However, for planets with small eccentricities, the ocean tides are much weaker but still comparable to that on modern Earth. Our results suggest that ocean tides on eccentric planets orbiting low-mass stars are orders of magnitude more powerful than those on Earth and can dramatically influence surface geography and orbital evolution.

[12] arXiv:2507.03906 [中文pdf, pdf, html, 其他]

标题： 行星系统的动力学演化半解析模型 II：应用于由行星形成模型形成的系统 显示英文标题

标题： Semi-analytical model for the dynamical evolution of planetary system II: Application to systems formed by a planet formation model

Tadahiro Kimura, Eiichiro Kokubo, Yuji Matsumoto, Christoph Mordasini, Masahiro Ikoma

评论： 11页，7图，已接受发表于ApJ

主题： 地球与行星天体物理学 (astro-ph.EP)

紧密的低质量行星的标准形成模型涉及高效的向内迁移，随后在原行星气体盘消散后通过巨大撞击增长。 虽然详细的N体模拟增强了我们的理解，但其高计算成本限制了与观测结果的统计比较。 在我们之前的工作中，我们引入了一个半解析模型，以跟踪气体盘消散后多个行星通过引力散射和巨大撞击的动力学演化。 尽管该模型在各种初始条件下成功再现了N体模拟结果，但我们的验证仍仅限于紧凑且等距排列的行星系统。 在本文中，我们改进了模型，以处理具有更广泛行星质量、半长轴和轨道分离变化的多样化行星系统，并将其与最近的行星种群合成结果进行验证。 我们增强的模型准确再现了最终行星系统的质量分布和轨道结构。 因此，我们确认该模型可以预测气体盘消散后的动力学演化结果，在广泛的行星系统结构中，这对于降低行星形成模拟的计算成本至关重要。 显示英文摘要

The standard formation model of close-in low-mass planets involves efficient inward migration followed by growth through giant impacts after the protoplanetary gas disk disperses. While detailed N-body simulations have enhanced our understanding, their high computational cost limits statistical comparisons with observations. In our previous work, we introduced a semi-analytical model to track the dynamical evolution of multiple planets through gravitational scattering and giant impacts after the gas disk dispersal. Although this model successfully reproduced N -body simulation results under various initial conditions, our validation was still limited to cases with compact, equally-spaced planetary systems. In this paper, we improve our model to handle more diverse planetary systems characterized by broader variations in planetary masses, semi-major axes, and orbital separations and validate it against recent planet population synthesis results. Our enhanced model accurately reproduces the mass distribution and orbital architectures of the final planetary systems. Thus, we confirm that the model can predict the outcomes of post-gas disk dynamical evolution across a wide range of planetary system architectures, which is crucial for reducing the computational cost of planet formation simulations.

[13] arXiv:2507.03968 [中文pdf, pdf, html, 其他]

标题： 地球的水是在太阳系形成最早阶段本地获得的吗？ 显示英文标题

标题： Was Earth's water acquired locally during the earliest phases of the Solar System formation?

Lise Boitard-Crépeau, Cecilia Ceccarelli, Pierre Beck, Lionel Vacher, Piero Ugliengo

评论： 7页，2图，发表于ApJL

期刊参考： 天体物理期刊快报 987 (2025) L25

主题： 地球与行星天体物理学 (astro-ph.EP)

地表水的起源仍然存在争议，因为标准的太阳系形成模型表明，地球是由干性颗粒形成的，位于原太阳星云的雪线之内。 在此，我们通过计算化学的角度重新审视这一问题。 虽然经典使用的雪线依赖于单一的冷凝温度，但量子化学的最新研究表明，水在冰性颗粒上的结合能呈高斯分布，这意味着水的升华是一个渐进的过程，而不是一个尖锐的转变。 我们利用计算得到的结合能分布来估计原太阳星云原行星盘中尘埃颗粒上吸附冰的径向分布。 我们的模型再现了地球上估计的全部范围的水丰度，并与预测形成距离的球粒陨石组的水化趋势相吻合。 因此，我们认为地球的大量水分可能是在太阳系形成早期阶段本地获得的，而无需从经典雪线之外输送而来。 显示英文摘要

The origin of the terrestrial water remains debated, as standard Solar System formation models suggest that Earth formed from dry grains, inside the snowline of the Proto-Solar Nebula (PSN). Here, we revisit this issue through the lens of computational chemistry. While the classically used snowline relies on a single condensation temperature, recent work in quantum chemistry shows that the binding energy of water on icy grains has a gaussian distribution, which implies a gradual sublimation of water rather than a sharp transition. We use the computed distribution of binding energies to estimate the radial distribution of adsorbed ice on the dust grains across the PSN protoplanetary disk. Our model reproduces the full range of estimated water abundances on Earth and matches the hydration trends observed in chondrite groups at their predicted formation distances. Thus, we suggest that a significant fraction of Earth's water may have been acquired locally at early stages of the Solar System formation, without requiring delivery from beyond the classical snowline.

[14] arXiv:2507.04291 [中文pdf, pdf, html, 其他]

标题： 与MAROON-X揭示的对齐次海王星以及小行星的对齐趋势 显示英文标题

标题： An Aligned Sub-Neptune Revealed with MAROON-X and a Tendency Towards Alignment for Small Planets

Alex S. Polanski, Ian J.M. Crossfield, Andreas Seifahrt, Jacob L. Bean, Jonathan Brande, Karen A. Collins, David R. Coria, Akihiko Fukui, Norio Narita, Julian Stürmer, Steven Giacalone, David Kasper

主题： 地球与行星天体物理学 (astro-ph.EP)

我们展示了使用MAROON-X对亚海王星TOI-1759A b的Rossiter-McLaughlin测量。与MuSCAT3测光数据和九次额外的TESS凌日数据联合分析得出天空投影的偏角为$|\lambda|$=$4^\circ\pm18^{\circ}$。我们还推导出真实的偏角为$\psi$=24$\pm12^{\circ}$，使该行星与完全对齐一致，尽管是到$<1\sigma$。具有18.85天的周期和40的$a/R_{*}$，TOI-1759A b是已测量偏角的最长周期单一亚海王星。它加入了越来越多的较小行星，这些行星已经进行了此测量，并且与K2-25 b一起，是目前唯一已知的单一且对齐的亚海王星。 我们还提供了对行星偏心率测量分布的概述，这些行星的半径为 R$<8$ R$_{\oplus}$。 我们发现这类行星倾向于对齐，特别是亚海王星和超级地球，这表明其形成历史是动态冷却的。 该类别中不对齐的行星大部分具有 4$<$R$\leq$8 R$_{\oplus}$，并且比处于紧凑系统中的行星更可能是孤立的。 我们发现这一结果在$3\sigma$水平上具有显著性，与之前的研究一致。 此外，我们在可用的档案径向速度数据上进行了注入和恢复测试，以限制这些系统中大伴星的存在。 目前的档案数据对于大多数系统来说不足以检测到巨行星。 显示英文摘要

We present the Rossiter-McLaughlin measurement of the sub-Neptune TOI-1759A b with MAROON-X. A joint analysis with MuSCAT3 photometry and nine additional TESS transits produces a sky-projected obliquity of $|\lambda|$= $4^\circ\pm18^{\circ}$. We also derive a true obliquity of $\psi$=24$\pm12^{\circ}$ making this planet consistent with full alignment albeit to $<1\sigma$. With a period of 18.85 days and an $a/R_{*}$ of 40, TOI-1759A b is the longest period single sub-Neptune to have a measured obliquity. It joins a growing number of smaller planets which have had this measurement made and, along with K2-25 b, is the only single, aligned sub-Neptune known to date. We also provide an overview of the emerging distribution of obliquity measurements for planets with R$<8$ R$_{\oplus}$. We find that these types of planets tend toward alignment, especially the sub-Neptunes and super-Earths implying a dynamically cool formation history. The majority of misaligned planets in this category have 4$<$R$\leq$8 R$_{\oplus}$ and are more likely to be isolated than planets rather than in compact systems. We find this result to be significant at the $3\sigma$ level, consistent with previous studies. In addition, we conduct injection and recovery testing on available archival radial velocity data to put limits on the presence of massive companions in these systems. Current archival data is insufficient for most systems to have detected a giant planet.

[15] arXiv:2507.04440 [中文pdf, pdf, html, 其他]

标题： 探索位于扩展适居带内的系外行星的适居性和内部组成 显示英文标题

标题： Exploring the habitability and interior composition of exoplanets lying within the extended habitable zone

Sushmita Deb, Kaushal Sharma, Samrat Biswas, Biman Jyoti Medhi

评论： 15页，6图

主题： 地球与行星天体物理学 (astro-ph.EP)

研究系外行星的可居住性、内部结构和组成对于理解它们在我们太阳系之外维持生命的可能性至关重要。表征行星结构和大气演化为了解表面条件和这些行星的长期可居住性提供了有价值的见解。在本研究中，我们对从超级地球到迷你海王星（$R_{\textrm{p}}$ $\leq$ 4$R_{\oplus}$和$M_{\textrm{p}}$ $\leq$ 15$M_{\oplus}$）进行了全面分析，这些行星位于扩展的适居带内，同时还对它们的主恒星进行了参数化。我们发现样本中的行星围绕红矮星运行并与之潮汐锁定。利用来自盖亚、Pan-STARRS1、2MASS和WISE的档案测光数据，我们估计了主恒星的大气和物理参数。我们还模拟了这些行星的内部结构以推断其可能的组成。此外，在假设这些系外行星可以吸积气体层的前提下，我们模拟了适居系外行星的包层比例。具有类似地球的岩石成分，LHS 1140 b和TOI-1452 b能够保留其初始气体层的微不足道量。然而，随着时间的推移维持足够的大气，LP 791-18 c、LTT 3780 c和K2-18 b很可能成为水世界。模型表明TOI-1266 c具有富含水的组成，而没有显著的大气层。模拟内部组成和大气逃逸情景使我们能够通过评估地表液态水的可能性和稳定大气的保持来评估这些行星的潜在可居住性。 显示英文摘要

Studying the habitability, internal structure and composition of exoplanets is crucial for understanding their potential to sustain life beyond our solar system. Characterizing planetary structures and atmospheric evolution provides valuable insights into surface conditions and the long-term habitability of these planets. In this study, we present a comprehensive analysis of exoplanets spanning from super-Earths to mini-Neptunes ($R_{\textrm{p}}$ $\leq$ 4 $R_{\oplus}$ and $M_{\textrm{p}}$ $\leq$ 15 $M_{\oplus}$) located within the extended habitable zone, along with parameterization of their host stars. We find that the planets in our sample orbit M dwarf stars and are tidally locked to them. Using archival photometric data from Gaia, Pan-STARRS1, 2MASS, and WISE, we estimate the atmospheric and physical parameters of the host stars. We also model the interior structure of these planets to infer their possible compositions. Additionally, under the assumption that these exoplanets can accrete a gaseous layer, we model the envelope fraction of the habitable exoplanets. With an Earth-like rocky composition, LHS 1140 b and TOI-1452 b can hold onto negligible amount of their initial gas layer. However, sustaining a sufficient amount of atmosphere over time, the planets LP 791-18 c, LTT 3780 c and K2-18 b are likely to be water worlds. The models suggest a water rich composition for TOI-1266 c without any significant amount of atmosphere. Modeling interior compositions and atmospheric escape scenarios allow us to assess the potential habitability of these planets by evaluating the likelihood of surface liquid water and the retention of stable atmospheres.

[16] arXiv:2507.04739 [中文pdf, pdf, html, 其他]

标题： 轨道转移优化连接弹道捕获到地月周期轨道族 显示英文标题

标题： Optimization of Transfers linking Ballistic Captures to Earth-Moon Periodic Orbit Families

Lorenzo Anoè, Roberto Armellin, Jack Yarndley, Thomas Caleb, Stéphanie Lizy-Destrez

主题： 地球与行星天体物理学 (astro-ph.EP) ; 动力系统 (math.DS) ; 数值分析 (math.NA) ; 优化与控制 (math.OC)

在NASA的阿尔忒弥斯计划和中国国家航天局的嫦娥计划背景下，地球-月球系统中周期轨道的转移设计再次受到重视。 本研究解决了将弹道捕获轨迹（利用多体动力学实现临时月球轨道插入）与圆限制三体问题（CR3BP）中描述的有界周期运动相连接的问题。 开发了一个统一的框架，通过CR3BP动力学的高阶多项式展开来优化双脉冲转移到周期轨道族。 同样的展开方法构成了轨道族的连续“算盘”参数化方法，实现了快速瞄准和解析灵敏度。 首先处理了平面周期轨道族（Lyapunov L1和L2，以及远距离逆行轨道），然后扩展到空间轨道族，如蝴蝶形和晕轮L1/L2轨道，并特别关注近直立晕轮轨道（NRHOs）。 数值结果展示了低成本解决方案，并验证了该方法在设计月球任务中的适应性。 优化的轨迹可以为已有的低能量转移数据库提供信息，通过反映转移可行性及与特定周期轨道族之间动力学关系的详细成本分析来丰富该数据库。 最后，所提出的转移提供了可靠的初始猜测，便于快速优化，并可根据任务需求进一步调整。 显示英文摘要

The design of transfers to periodic orbits in the Earth--Moon system has regained prominence with NASA's Artemis and CNSA's Chang'e programs. This work addresses the problem of linking ballistic capture trajectories - exploiting multi-body dynamics for temporary lunar orbit insertion - with bounded periodic motion described in the circular restricted three-body problem (CR3BP). A unified framework is developed for optimizing bi-impulsive transfers to families of periodic orbits via a high-order polynomial expansion of the CR3BP dynamics. That same expansion underlies a continuous 'abacus' parameterization of orbit families, enabling rapid targeting and analytic sensitivity. Transfers to planar periodic-orbit families (Lyapunov L1 and L2, and distant retrograde orbits) are addressed first, followed by extension to spatial families, such as butterfly and halo L1/L2 orbits, with an emphasis towards Near-Rectilinear Halo Orbits (NRHOs). Numerical results demonstrate low-cost solutions and validate the method's adaptability for the design of lunar missions. The optimized trajectories can inform an established low-energy transfer database, enriching it with detailed cost profiles that reflect both transfer feasibility and underlying dynamical relationships to specific periodic-orbit families. Finally, the proposed transfers provide reliable initial guesses for rapid refinement, readily adaptable for further optimization across mission-specific needs.

[17] arXiv:2507.04954 [中文pdf, pdf, html, 其他]

标题： 卫星在致密固态粒子盘中的形成 显示英文标题

标题： On the formation of satellites in dense solid-particle disks

G. Madeira, L. Esteves, T.F.L.L. Pinheiro, P.V.S. Soares, N.S. Santos, B. Morgado

评论： 被接受于《行星与空间科学》

主题： 地球与行星天体物理学 (astro-ph.EP)

单个大卫星具有重要的观测兴趣，因为它们可以产生显著且可能可检测的特征。 对于类地行星和超级地球来说，形成晚期的巨大撞击可能会产生致密的自引力盘——有利于此类卫星形成的有利环境。 受此启发，我们通过三维N体模拟研究致密固态粒子盘中的卫星形成，重点研究盘质量以及表面密度指数的影响。 我们的结果揭示了在相同盘参数下形成的卫星质量和配置存在显著变化，突显了这一过程的随机性。 更高的盘质量和更平坦的表面密度分布有利于形成更高质量的卫星。 质量高于0.03行星质量的盘通常会产生一个主导卫星，而质量在0.003到0.03之间的盘则倾向于形成双卫星系统。 平均而言，最大卫星的质量与初始盘质量成线性关系，这与分析预测一致。 我们估计，围绕一颗1.6倍地球质量的行星运行的最小质量为0.03行星质量的盘，可能形成一个类似地月系统的卫星，该系统可通过具有10百万分率光度精度的望远镜探测到——这一水平是詹姆斯·韦伯空间望远镜可实现的。 显示英文摘要

Single massive satellites are of great observational interest, as they can produce prominent and potentially detectable signatures. For terrestrial planets and super-Earths, giant impacts in the late stages of formation may generate dense self-gravitating disks - favourable environments for the formation of such satellites. Motivated by this, we explore satellite formation in dense solid-particle disks through three-dimensional N-body simulations, focusing on the effects of disk mass and the surface density exponent. Our results reveal significant variability in the masses and configurations of satellites formed under identical disk parameters, highlighting the stochastic nature of the process. Higher disk masses and flatter surface density profiles favour the formation of more massive satellites. Disks with masses above 0.03 planetary masses typically yield a single dominant satellite, while those between 0.003 and 0.03 tend to form two-satellite systems. On average, the mass of the largest satellite scales linearly with the initial disk mass, in agreement with analytical predictions. We estimate that a disk with a minimal mass of 0.03 planetary masses around a 1.6 Earth-mass planet orbiting a Sun-like star could form an Earth-Moon-like system detectable by telescopes with a photometric precision of 10 parts per million - a level achievable by the James Webb Space Telescope.

[18] arXiv:2507.04987 [中文pdf, pdf, html, 其他]

标题： 关于太阳系N体模拟的收敛性 显示英文标题

标题： On the convergence of N-body simulations of the Solar System

Hanno Rein, Garett Brown, Mei Kanda

评论： 5页，3图，提交至OJA

主题： 地球与行星天体物理学 (astro-ph.EP) ; 天体物理学的仪器与方法 (astro-ph.IM) ; 数值分析 (math.NA)

大多数行星系统的直接N体积分使用固定时间步长的对称积分器。 较大的时间步长是理想的，因为模拟运行速度快。 然而，如果时间步长太大，模拟结果会变得不物理。 令人惊讶的是，尚未在长期（十亿年）时间尺度上进行过系统性的收敛研究。 在本文中，我们进行了数值实验，以确定在长期积分中必须使用的最小时间步长，以便恢复太阳系的基本长期频率和不稳定率。 我们发现，最多32天的时间步长，即水星轨道周期的三分之一，在50亿年的积分中会产生物理结果。 我们认为，驱动太阳系长期演化的混沌扩散超过了数值扩散和时间步长共振。 我们的结果增强了对文献中大多数模拟确实收敛的信心，并提供了如何运行时间和能量高效的模拟的指导，同时确保结果可以信赖。 显示英文摘要

Most direct N-body integrations of planetary systems use a symplectic integrator with a fixed timestep. A large timestep is desirable because simulations run fast. However, simulations yield unphysical results if the timestep is too large. Surprisingly, no systematic convergence study has been performed on long (Gyr) timescales. In this paper we present numerical experiments to determine the minimum timestep one has to use in long-term integrations of the Solar System in order to recover the system's fundamental secular frequencies and instability rate. We find that timesteps of up to 32 days, i.e. a third of Mercury's orbital period, yield physical results in 5 Gyr integrations. We argue that the chaotic diffusion that drives the Solar System's long-term evolution dominates over numerical diffusion and timestep resonances. Our results bolster confidence that most simulations in the literature are indeed converged and provide guidance on how to run time and energy efficient simulations while making sure results can be trusted.

[19] arXiv:2507.05051 [中文pdf, pdf, html, 其他]

标题： 一颗在近日点附近的NH$_2$丰富的星际彗星 2I/Borisov 的画像 显示英文标题

标题： A portrait throughout perihelion of the NH$_2$-rich interstellar comet 2I/Borisov

Sophie E. Deam, Michele T. Bannister, Cyrielle Opitom, Matthew M. Knight, Ryan Ridden-Harper, Darryl Z. Seligman, Alan Fitzsimmons, Aurélie Guilbert-Lepoutre, Emmanuel Jehin, Laurent Jorda, Michael Marsset, Youssef Moulane, Philippe Rousselot, Pierre Vernazza, Bin Yang

评论： 提交至PSJ，欢迎提出意见

主题： 地球与行星天体物理学 (astro-ph.EP) ; 星系的天体物理学 (astro-ph.GA)

星际彗星2I/Borisov是第一个在其整个近日点通过过程中能够进行成分表征的星际物体。 我们报告了使用ESO VLT的积分场光谱仪MUSE进行的全面光学观测活动的所有16个时相，时间跨度为126天，从2019年11月14日到2020年3月19日。 2I/Borisov的空间尘埃发射主要平滑，没有季节性影响。 一个类似喷流的特征一直可见。 其彗发的气体生成形态也是平滑的，对于C$_2$，NH$_2$和CN来说，围绕光中心对称。 这些物质的生成率在近日点前后逐渐下降，直到2I在2020年3月初爆发和分裂事件。 C$_2$，NH$_2$和 CN的生成率都增加了，其中NH$_2$增加最为显著；尘埃发射也略微变红。 与太阳系中迄今测量的彗星相比，2I/Borisov是一个碳贫乏、相对NH$_2$含量丰富的彗星。 显示英文摘要

The interstellar comet 2I/Borisov is the first interstellar object where compositional characterisation was possible throughout its entire perihelion passage. We report all 16 epochs of a comprehensive optical observation campaign with ESO VLT's integral field spectrograph MUSE, spanning 126 days from 2019 November 14 to 2020 March 19. The spatial dust emission of 2I/Borisov was predominantly smooth, with no seasonal effect. A jet-like feature was consistently visible. The gas production morphology of its coma was also smooth and similar for C$_2$, NH$_2$, and CN: symmetric around the photocentre. The production rates of these species gently declined into and beyond perihelion, until 2I's outburst and splitting event in early 2020 March. C$_2$, NH$_2$, and CN production rates all increased, with NH$_2$ being the most significant; the dust emission also slightly reddened. 2I/Borisov is a carbon-depleted, relatively NH$_2$-rich comet when compared to those comets yet measured in the Solar System.

[20] arXiv:2507.05090 [中文pdf, pdf, html, 其他]

标题： 白矮星轨道上小行星的破坏时间尺度的二进制灾难限制 显示英文标题

标题： Bounding destruction timescales of minor planets orbiting white dwarfs with the sesquinary catastrophe

Dimitri Veras, Matija Ćuk

评论： 已接受发表于MNRAS

主题： 地球与行星天体物理学 (astro-ph.EP) ; 太阳与恒星天体物理学 (astro-ph.SR)

围绕白矮星运行的小行星的破坏引起的动态活动现在已经通过光度监测在个别系统中持续了长达十年，足以测量到明显的中断和重新出现的凌日特征。 此外，暗示白矮星洛希半径外部存在碎片的周期性现象，以及对碎片盘寿命的广泛估计（高达百万年），使这些系统的形成和动态演化理论变得复杂。 在这里，我们说明了轨道周期为$\approx$5-25小时及更长、完全或部分避免潮汐破坏的围绕白矮星运行的小行星满足发生 sesquinary 灾难的条件，这是一种在太阳系中当从月球返回的喷射物撞击速度足够快以至于造成侵蚀并最终破坏的现象。 因此，我们发现对应于$\approx$1-4个白矮星碎石堆洛希半径的区域是一个危险区域，sesquinary 灾难发生的碰撞时间尺度为$\sim 10^2-10^5$年，这表明白矮星周围的碎片盘处于半连续补充的状态。 显示英文摘要

Dynamical activity attributed to the destruction of minor planets orbiting white dwarfs has now been photometrically monitored in individual systems for up to one decade, long enough to measure significant cessation and re-emergence of transit features. Further, periodicities which hint at the presence of debris orbiting exterior to the white dwarf Roche radius, along with widely varying estimates for debris disc lifetimes (up to Myrs), complicate theories for the formation and dynamical evolution of these systems. Here, we illustrate that minor planets orbiting white dwarfs with periods of $\approx$5-25 hours and longer while completely or partially avoiding tidal disruption satisfy the conditions for the occurrence of the sesquinary catastrophe, a phenomenon that occurs in the solar system when impacts from returning ejecta from a moon are fast enough to be erosional to the point of destruction. We hence find that the region corresponding to $\approx$1-4 white dwarf rubble-pile Roche radii represents a danger zone where the collisional timescale for the sesquinary catastrophe to occur is $\sim 10^2-10^5$ yr, suggesting that debris discs around white dwarfs are in a state of semi-continuous replenishment.

[21] arXiv:2507.05109 [中文pdf, pdf, html, 其他]

标题： 核心侵蚀在气态巨行星中的能量视角 显示英文标题

标题： An Energy Perspective of Core Erosion in Gas Giant Planets

J. R. Fuentes, Christopher R. Mankovich, Ankan Sur

评论： 已接受发表于ApJ Letters

主题： 地球与行星天体物理学 (astro-ph.EP) ; 太阳与恒星天体物理学 (astro-ph.SR)

朱诺号和卡西尼号表明，木星和土星可能含有重元素的扩展梯度。 然而，这些梯度如何在数十亿年中存活仍然是一个开放问题。 经典对流理论预测快速混合和均质化，这将在远短于行星年龄的时间尺度上消除这些梯度。 为了解决这个问题，我们估计侵蚀致密核心和模糊核心所需的能量，并将其与行星实际能提供的能量进行比较。 如果整个冷却预算可用于驱动混合，则即使是一个紧凑的核心原则上也可以被破坏。 但如果混合仅限于核心附近的热能，这是另一种合理的场景，那么能量是不足的。 在这种情况下，木星可以侵蚀大约$10~\mearth$的模糊核心，但紧凑核心仍然完好无损。 土星的核心更为坚固。 即使在模糊情况下，也只有大约$1~\mearth$被损失，如果核心是紧凑的，侵蚀可以忽略不计。 结果对假设的初始温度和熵分布非常敏感。 更热且更超绝热的内部更容易发生混合。 我们认为，具有现实分层和足够深度（即许多密度标高）的从上而下的三维对流模拟将对进一步约束核心侵蚀的能量预算具有重要意义。 显示英文摘要

Juno and Cassini have shown that Jupiter and Saturn likely contain extended gradients of heavy elements. Yet, how these gradients can survive over billions of years remains an open question. Classical convection theories predict rapid mixing and homogenization, which would erase such gradients on timescales far shorter than the planets' ages. To address this, we estimate the energy required to erode both dense and fuzzy cores, and compare it to what the planet can realistically supply. If the entire cooling budget is available to drive mixing, then even a compact core can, in principle, be destroyed. But if mixing is limited to the thermal energy near the core, which is another plausible scenario, the energy falls short. In that case, Jupiter can erode a fuzzy core by up to approximately $10~\mearth$, but a compact one remains intact. Saturn's core is more robust. Even in the fuzzy case, only about $1~\mearth$ is lost, and if the core is compact, erosion is negligible. The outcome depends sensitively on the assumed initial temperature and entropy profiles. Hotter and more superadiabatic interiors are more prone to mixing. We suggest that 3D simulations of convection driven from above, with realistic stratification and enough depth (i.e., many density scale heights) would be of great interest to further constrain the energy budget for core erosion.

[22] arXiv:2507.05155 [中文pdf, pdf, html, 其他]

标题： 詹姆斯·韦布空间望远镜对自由漂浮的行星质量天体及其盘的光谱学研究 显示英文标题

标题： Spectroscopy of Free-Floating Planetary-Mass Objects and their disks with JWST

Belinda Damian, Aleks Scholz, Ray Jayawardhana, V. Almendros-Abad, Laura Flagg, Koraljka Mužić, Antonella Natta, Paola Pinilla, Leonardo Testi

评论： 已被《天文学杂志》接受发表。15页，11幅图，1张表

主题： 地球与行星天体物理学 (astro-ph.EP) ; 星系的天体物理学 (astro-ph.GA)

已知自由漂浮的行星质量天体（FFPMOs）在年轻年龄时拥有盘。在此，我们展示了八个年轻FFPMOs的1-13$\mu m$光谱，这些天体的质量为5-10 M$_\mathrm{Jup}$ （年龄为1-5 Myr），使用詹姆斯·韦布空间望远镜上的NIRSpec和MIRI仪器。我们推导了这些目标的基本特性，并发现光谱类型为M9.5到L4，有效温度为1600-1900 K。我们目标的光球光谱在相似温度下显示出明显的多样性，特别是在3-5$\mu m$范围内，这无法用现有的大气模型解释。我们在其中一个目标的光球中发现了硅酸盐吸收特征，这是非常年轻的FFPMOs中的首次检测，表明它们的冷大气中有硅酸盐云。我们的六个物体在光球之上显示出中红外过量辐射，以及硅酸盐发射特征，证明了盘的存在。后者的特征形状和强度构成了颗粒增长和结晶的有力证据，类似于在更高质量的棕矮星和恒星中所见的情况。我们还在几个目标的盘中检测到了碳氢化合物分子的发射线。这些是迄今为止发现的质量最低的孤立天体，其盘中出现了硅酸盐和碳氢化合物的发射特征。盘的存在及其特征表明，在自由漂浮的行星质量天体周围有可能形成岩石伴星。 显示英文摘要

Free-floating planetary-mass objects (FFPMOs) are known to harbor disks at young ages. Here, we present 1-13 $\mu m$ spectra for eight young FFPMOs with masses of 5-10 M$_\mathrm{Jup}$ (at ages of 1-5 Myr), using the NIRSpec and MIRI instruments on the James Webb Space Telescope. We derive fundamental properties of these targets, and find spectral types of M9.5 to L4, with effective temperatures of 1600-1900 K. The photospheric spectra of our targets show a clear diversity at similar temperatures, especially in the 3-5 $\mu m$ range, unaccounted for by existing atmospheric models. We find a silicate absorption feature in the photosphere of one of our targets, the first such detection in very young FFPMOs, indicating silicate clouds in their cool atmospheres. Six of our objects show mid-infrared excess emission above the photosphere, as well as silicate emission features, demonstrating the presence of disks. The shape and strength of the latter features constitute strong evidence of grain growth and crystallization, similar to what is seen in more massive brown dwarfs and stars. We also detect emission lines from hydrocarbon molecules in the disks of several targets. These are the lowest mass isolated objects found so far with silicate and hydrocarbon emission features arising in their disks. The presence of disks and their characteristics point to the potential for the formation of rocky companions around free-floating planetary-mass objects.

[23] arXiv:2507.05202 [中文pdf, pdf, html, 其他]

标题： 罗斯比数区域，对流抑制和膨胀热木星中的发电机磁性 显示英文标题

标题： Rossby number regime, convection suppression, and dynamo-generated magnetism in inflated hot Jupiters

Albert Elias-López, Matteo Cantiello, Daniele Viganò, Fabio Del Sordo, Simranpreet Kaur, Clàudia Soriano-Guerrero

评论： （例如：20页，10图，已被Apj接收）

主题： 地球与行星天体物理学 (astro-ph.EP)

热木星（HJs）通常被认为在系外行星中拥有最强的由发电机效应产生的磁场，其强度比木星高一个数量级。因此，它们经常被视为最有可能显示磁星-行星相互作用信号和磁驱动的相干射电辐射的系外行星，尽管进行了多种多样的观测活动，但这一现象仍然难以捉摸。在这项工作中，我们通过一维模型研究了热木星内部对流和发电机特性的演化。我们探讨了轨道距离、行星和恒星质量以及热量注入类型的影响。我们采用一维演化模型来获得内部对流结构。具体而言，在证明潮汐同步对于所有热木星都可能有效之后，我们得到了罗斯比数$\mathrm{Ro}$作为行星深度和轨道周期的函数。当热量均匀施加时，几乎所有热木星的对流层仍处于快速旋转器状态，$\mathrm{Ro} \lesssim 0.1$，除了质量最大的行星且轨道距离较大（但仍被潮汐锁定）。我们通过应用已知的快速旋转器的标度定律来恢复膨胀热木星的磁场强度。当强热源主要施加在外部包层和发电机区域之外时，如现实的欧姆模型所预测的那样，发电机区域的对流通常会崩溃。因此，热通量和推导出的表面磁场可能会大大降低至或低于木星值，这与通常的假设相反，从而对相干射电辐射的估计产生负面影响，并可能解释到目前为止未能检测到它的原因。 显示英文摘要

Hot Jupiters (HJs) are commonly thought to host the strongest dynamo-generated magnetic fields among exoplanets, up to one order of magnitude larger than Jupiter. Thus, they have often been regarded as the most promising exoplanets to display magnetic star-planet interaction signals and magnetically-driven coherent radio emission, which unfortunately remains elusive, despite many diversified observational campaigns. In this work, we investigate the evolution of the internal convection and dynamo properties of HJs via one-dimensional models. We explore the dependency on orbital distance, planetary and stellar masses, and types of heat injection. We employ one-dimensional evolutionary models to obtain internal convective structures. Specifically, we obtain the Rossby number $\mathrm{Ro}$ as a function of planetary depth and orbital period, after showing that tidal synchronization is likely valid for all HJs. When the heat is applied uniformly, the convective layers of almost all HJs remain in the fast rotator regime, $\mathrm{Ro} \lesssim 0.1$, except possibly the most massive planets with large orbital distances (but still tidally locked). We recover magnetic field strengths for inflated HJs by applying well-known scaling laws for fast rotators. When strong heat sources are applied mostly in the outer envelope and outside the dynamo region, as realistic Ohmic models predict, convection in the dynamo region often breaks down. Consequently, the heat flux and the derived surface magnetic fields can be greatly reduced to or below Jovian values, contrary to what is commonly assumed, thus negatively affecting estimates for coherent radio emission, and possibly explaining the failure in detecting it so far.

[24] arXiv:2507.05226 [中文pdf, pdf, html, 其他]

标题： 3I/ATLAS星际物体的初始VLT/MUSE光谱观测 显示英文标题

标题： Initial VLT/MUSE spectroscopy of the interstellar object 3I/ATLAS

Cyrielle Opitom, Colin Snodgrass, Emmanuel Jehin, Michele T. Bannister, Erica Bufanda, Sophie E. Deam, Rosemary Dorsey, Marin Ferrais, Said Hmiddouch, Matthew M. Knight, Rosita Kokotanekova, Brayden Leicester, Michaël Marsset, Brian Murphy, Vincent Okoth, Ryan Ridden-Harper, Mathieu Vander Donckt, Léa Ferellec, Damien Hutsemekers, Manuela Lippi, Jean Manfroid, Zouhair Benkhaldoun

评论： 提交至MNRAS

主题： 地球与行星天体物理学 (astro-ph.EP) ; 星系的天体物理学 (astro-ph.GA)

星际彗星3I/ATLAS是第三个被发现的星际物体。 近日点前的测量提供了一个独特的机会来研究它的活动和成分，这些可能在接下来的几个月中因受热而发生变化。 我们提供了光学光谱观测的初步基准，这些观测是在发现后仅两天使用VLT上的MUSE仪器于2025年7月3日进行的，当时3I距离太阳4.47天文单位，距离地球3.46天文单位。 这些观测证实了3I的彗星性质，并揭示了一个红色的彗发，其光谱斜率为$(18\pm4)\%/1000$~\AA ，比大多数太阳系彗星更红，但与一些太阳系海王星外天体或半人马小行星的表面颜色相似。 我们搜索了C$_2$、NH$_2$、CN和[OI]的气体发射，但未检测到，这与在这一日心距离下太阳系彗星的挥发性物质未检测到一致。 目前，彗发似乎完全是尘埃组成的。 随着3I逐渐接近太阳，未来的观测将提供一个无价的机会来观察其活动性的演变，研究其成分，测试星际物体种群模型的预测，并将3I与太阳系彗星进行比较。 显示英文摘要

The interstellar comet 3I/ATLAS is only the third interstellar object to be discovered. Pre-perihelion measurements provide a unique opportunity to study its activity and composition, which may alter as it is heated in the coming months. We provide an initial baseline from optical spectroscopic observations obtained only two days after discovery, using the MUSE instrument on the VLT on 2025 July 3, while 3I was at 4.47 au from the Sun and 3.46 au from the Earth. These observations confirm the cometary nature of 3I, and reveal a red coma with a spectral slope of $(18\pm4)\%/1000$~\AA, redder than most Solar System comets but similar to the surface colour of some Solar System Trans-Neptunian Objects or Centaurs. We searched for but did not detect gas emission from C$_2$, NH$_2$, CN, and [OI], which is consistent with volatile non-detections for Solar System comets at this heliocentric distance. At present, the coma appears entirely dusty. Future observations of 3I as it comes closer to the Sun will provide an invaluable opportunity to witness the evolution of its activity, study its composition, test predictions of interstellar object population models, and compare 3I to Solar System comets.

[25] arXiv:2507.05252 [中文pdf, pdf, html, 其他]

标题： 星际彗星3I/ATLAS：发现和物理描述 显示英文标题

标题： Interstellar comet 3I/ATLAS: discovery and physical description

Bryce T. Bolin, Matthew Belyakov, Christoffer Fremling, Matthew J. Graham, Candace L. Gray, Carl Ingebretsen, Gracyn Jewett, Mukremin Kilic, Carey M. Lisse, Diana Roderick, Ahmed. M. Abdelaziz, Laura-May Abron, Michael W. Coughlin, Eslam Elhosseiny, Cheng-Han Hsieh, Martin Mašek, Mona Molham, Ali Takey, Keith S. Noll, Ian Wong

评论： 8页，4图，2表，提交至MNRAS:L

主题： 地球与行星天体物理学 (astro-ph.EP) ; 星系的天体物理学 (astro-ph.GA) ; 天体物理学的仪器与方法 (astro-ph.IM)

我们描述了星际彗星3I\ATLAS 的物理特性，该彗星于2025年7月1日由小行星地球撞击最后预警系统发现。 彗星的偏心率，$e$ $\simeq$ 6.08 和无限远处的速度，v$_{\infty}$ $\simeq$ 57 km/s，表明其具有星际起源。 我们在2025年7月3日使用帕洛马200英寸下一代帕洛马光谱仪获得了g、r、i测光数据。 我们测量了颜色指数 g-r = 0.43$\pm$0.02 mag，r-i = 0.16$\pm$0.02 mag，以及 g-i = 0.59$\pm$0.03 mag 和光谱斜率为 1.3$\pm$0.9$\%$/100 nm。 我们计算了彗星 10,000 km 范围内的尘埃截面为 230.0$\pm$5.2 km$^2$，假设反照率为 0.10。 3I\ATLAS 的检测 FWHM 为$\sim$2.2 角秒，在我们的 r 波段图像中测量得到，其 A(0$^\circ$)f$\rho$为 287.2$\pm$2.8 平方厘米。 最后，我们利用彗发的朝向太阳的范围来限制尘埃喷射速度，发现\textmu 量级的颗粒具有$\sim$0.01-1 m/s，这意味着彗星的尘埃质量损失率是$\sim$0.1 - 1.0 kg/s. 显示英文摘要

We describe the physical characteristics of interstellar comet 3I\ATLAS, discovered on 2025 July 1 by the Asteroid Terrestrial-impact Last Alert System. The comet has eccentricity, $e$ $\simeq$ 6.08 and velocity at infinity, v$_{\infty}$ $\simeq$ 57 km/s, indicating an interstellar origin. We obtained g, r, i photometry with the Palomar 200-inch Next Generation Palomar Spectrograph on 2025 July 3. We measured colour indices g-r = 0.43$\pm$0.02 mag, r-i = 0.16$\pm$0.02 mag, and g-i = 0.59$\pm$0.03 mag and a spectral slope of 1.3$\pm$0.9 $\%$/100 nm. We calculate the dust cross-section within 10,000 km of the comet to be 230.0$\pm$5.2 km$^2$, assuming an albedo of 0.10. The FWHM of 3I\ATLAS's detection is $\sim$2.2 arcsec as measured in our r-band images and has A(0$^\circ$)f$\rho$ of 287.2$\pm$2.8 cm. Finally, we use the sunward extent of the coma to constrain the dust ejection speed, finding that \textmu m-scale to mm-scale particles have $\sim$0.01-1 m/s, implying the comet's dust mass-loss rate is $\sim$0.1 - 1.0 kg/s.

交叉提交 (展示 7 之 7 条目 )

[26] arXiv:2507.03029 (交叉列表自 astro-ph.IM) [中文pdf, pdf, html, 其他]

标题： 白矮星作为系外行星成分和基本天体物理学的探针 显示英文标题

标题： White dwarfs as probes of extrasolar planet compositions and fundamental astrophysics

Siyi Xu, Martin Barstow, Andy Buchan, Érika Le Bourdais, Patrick Dufour

评论： 11页；7图；将发表于HWO2025会议的ASP会议论文集

主题： 天体物理学的仪器与方法 (astro-ph.IM) ; 地球与行星天体物理学 (astro-ph.EP) ; 太阳与恒星天体物理学 (astro-ph.SR)

白矮星代表恒星演化的最常见的最终阶段，并且对于一系列天体物理问题非常重要。 宜居世界观测台（HWO）的高分辨率紫外线光谱能力提供了独特的特性来表征白矮星。 在本文中，我们关注HWO的两个具体科学案例——白矮星作为太阳系外行星成分的探针，以及基本天体物理学。 HWO将具有灵敏度，在大量污染的白矮星中测量一系列重元素，如S、C、O、Fe和Si，以限制太阳系外行星核心中的水含量和轻元素。 HWO还可以用来在强引力存在的情况下搜索精细结构常数的任何微小变化。 这两个科学案例都需要最小的分辨率功率为60,000，并且紫外线覆盖范围至少达到900埃。 显示英文摘要

White dwarfs represent the most common end stage of stellar evolution and are important for a range of astrophysical questions. The high-resolution ultraviolet spectroscopic capability of the Habitable World Observatory (HWO) offers a unique capability to characterize white dwarfs. In this documents, we focus on two specific science cases for HWO -- white dwarfs as probes of extrasolar planet compositions, and fundamental astrophysics. HWO will have the sensitivity to measure a suite of heavy elements, such as S, C, O, Fe, and Si, in a large sample of polluted white dwarfs to constrain the water content and the light elements in the cores of extrasolar planets. HWO can also be used to search for any small variation on the fine structure constant in the presence of strong gravity. Both science cases require a minimum resolving power of 60,000, and a ultraviolet coverage down to at least 900 Angstrom.

[27] arXiv:2507.03060 (交叉列表自 astro-ph.IM) [中文pdf, pdf, html, 其他]

标题： 高分辨率紫外至近红外系外行星大气层表征 显示英文标题

标题： High-resolution Ultraviolet-to-nearinfrared Characterization of Exoplanet Atmospheres

Patricio E. Cubillos, Matteo Brogi, Antonio García Muñoz, Luca Fossati, Sudeshna Boro Saikia, Vincent Bourrier, Jose A. Caballero, Juan Cabrera, Andrea Chiavassa, Andrzej Fludra, Leonardos Gkouvelis, John Lee Grenfell, Manuel Guedel, Alvaro Labiano, Monika Lendl, Donna Rodgers-Lee, Arnaud Salvador, Ilane Schroetter, Antoine Strugarek, Benjamin Taysum, Aline Vidotto, Thomas G. Wilson

评论： 宜居世界天文台的科学案例开发文件。欢迎于2025年8月15日前提交评论和推荐信，邮箱：patricio.cubillos@oeaw.ac.at

主题： 天体物理学的仪器与方法 (astro-ph.IM) ; 地球与行星天体物理学 (astro-ph.EP)

宜居世界观测台（HWO）提供了一个独特的机会，以彻底改变我们对行星形成和演化的理解。 本科学案例开发文件（SCDD）的目标是研究塑造系外行星组成和大气质量损失的物理和化学过程。 我们回顾了目前通过凌日观测作为质量损失诊断的关键可观测量，即逃逸氢的吸收线（Lyman-alpha）、氦和金属（Fe、Mg、C、O）。 我们还探讨了基于大气成分表征推断行星形成过程的挑战。 HWO可以实现从远紫外到近红外光谱（~100--1600 nm）的广泛连续覆盖，分辨率高（R > 60, 000），这对于进行这些测量、区分其行星起源与恒星活动，并最终通过同时表征系外行星大气的成分、云层主导程度和热结构来确定逃逸率至关重要。 显示英文摘要

The Habitable Worlds Observatory (HWO) offers a unique opportunity to revolutionize our understanding of planetary formation and evolution. The goal of this Science Case Development Document (SCDD) is to investigate the physical and chemical processes that shape the composition and atmospheric mass loss in exoplanets. We review the key observables currently known as diagnostics of mass loss via transit observations, i.e., absorption lines of escaping hydrogen (Lyman-alpha), helium, and metals (Fe, Mg, C, O). We also explore the challenges to infer planetary formation processes based on atmospheric composition characterization. HWO could enable a broad, continuous coverage from far-ultraviolet to near-infrared spectroscopy (~100--1600 nm) at high resolution (R > 60, 000), which is essential to make these measurements, disentangle their planetary origin from stellar activity, and ultimately, contextualize the escape rates by simultaneously characterizing the composition, cloud predominance, and thermal structure of exoplanet atmospheres.

[28] arXiv:2507.03071 (交叉列表自 astro-ph.IM) [中文pdf, pdf, html, 其他]

标题： 检测系外行星表面液态水 显示英文标题

标题： Detecting Surface Liquid Water on Exoplanets

Nicolas B. Cowan, Jacob Lustig-Yaeger, Renyu Hu, Laura C. Mayorga, Tyler D. Robinson (on behalf of the Characterizing Exoplanets sub working group)

评论： 迈向宜居世界观测站：远见科学与变革性技术SCDD，将在HWO2025上发表，并在征求社区意见后提交至太平洋天文学会

主题： 天体物理学的仪器与方法 (astro-ph.IM) ; 地球与行星天体物理学 (astro-ph.EP)

有大量水体的行星将拥有更温和且稳定的气候，这样的行星是已知生命形式出现和进化的理想场所。宜居世界观测台（HWO）的一个关键科学目标是确定哪些行星拥有地表液态水。除了对行星气候和天体生物学的意义外，在类地系外行星上检测到地表水将对我们关于行星形成和挥发物输送的理论施加重要的限制。系外行星反射率的旋转变化可能揭示出随视图旋转进出的表面特征，包括海洋。同时，反射率和偏振的轨道变化对行星表面的散射相函数敏感，包括来自大面积水体的镜面反射。尽管这些技术适用于所有温带类地系外行星，但本文档重点关注那些更可能推动HWO日冕仪设计的直接成像行星。识别海洋依赖于检测液体，并利用其他证据将该液体缩小到是水。液体比大多数固体具有更平滑的表面，因此表现出镜面反射而非漫反射。实际上，这使得湖泊和海洋从大多数照明角度看起来很暗，但在倾斜角度下则像镜子一样。HWO能够通过其光学特性唯一地识别地表液态海洋。鉴于在系外行星上发现海洋将证实其作为宜居世界的资格，这个科学案例实际上是宜居世界观测台存在的根本原因。 显示英文摘要

Planets with large bodies of water on their surface will have more temperate and stable climates, and such planets are the ideal places for life-as-we-know-it to arise and evolve. A key science case for the Habitable Worlds Observatory (HWO) is to determine which planets host surface liquid water. Aside from its implications for planetary climate and astrobiology, detecting surface water on terrestrial exoplanets would place important constraints on our theories of planet formation and volatile delivery. Rotational variability in the reflectance of an exoplanet may reveal surface features rotating in and out of view, including oceans. Orbital changes in reflectance and polarization, meanwhile, are sensitive to the scattering phase function of the planetary surface, including specular reflection from large bodies of water. Although these techniques are applicable to all temperate terrestrial exoplanets, we focus in this document on the directly-imaged planets that are more likely to drive the HWO coronagraph design. Identification of water oceans relies on detecting a liquid, and using other lines of evidence to narrow that liquid down to being water. Liquids have smoother surfaces than most solids, and hence exhibit specular reflection instead of diffuse reflection. In practice, this makes lakes and oceans look dark from most illumination angles, but mirror-like at glancing angles. HWO is uniquely capable of identifying surface liquid oceans via their optical properties. Given that discovering an ocean on an exoplanet would confirm its status as a habitable world, this science case is literally the raison d'etre of the Habitable Worlds Observatory.

[29] arXiv:2507.03102 (交叉列表自 astro-ph.IM) [中文pdf, pdf, html, 其他]

标题： 构建SPARCS，一个用于系外行星可居住性研究、技术进步和任务培训的紫外科学立方星 显示英文标题

标题： Building SPARCS, an Ultraviolet Science CubeSat for Exoplanet Habitability Studies, Technology Advancements, and Mission Training

Evgenya L. Shkolnik, David R. Ardila, Logan Jensen, April D. Jewell, Tahina Ramiaramanantsoa, Judd Bowman, Daniel Jacobs, Paul Scowen, Christophe Basset, Johnathan Gamaunt, Dawn Gregory, Maria C. Ladwig, Matthew Kolopanis, Shouleh Nikzad, Nathaniel Struebel, Joe Llama, Mary Knapp, Sarah Peacock, Titu Samson, Mark Swain

评论： 已接受发表于《天文学望远镜、仪器和系统杂志》（JATIS）

主题： 天体物理学的仪器与方法 (astro-ph.IM) ; 地球与行星天体物理学 (astro-ph.EP)

星-行星活动研究立方卫星（SPARCS）是一项由美国国家航空航天局资助的6U立方卫星任务，旨在监测低质量恒星的紫外线（UV）辐射。这些恒星相对高频和高能的紫外线耀斑显著影响绕行系外行星的大气层，导致大气流失并改变适居条件。SPARCS旨在同时捕捉远紫外线和近紫外线的时间分辨光度数据，以更好地表征耀斑并检测最强和最罕见的耀斑。此外，SPARCS正在测试创新技术，如具有接近100%内部量子效率的delta掺杂探测器和集成金属电介质紫外线带通滤波器。该任务将提高这些关键组件的技术成熟度，使其适用于未来的旗舰任务，如宜居世界观测站。本文概述了SPARCS的任务目标，并提供了航天器完成后的更新信息，该航天器预计于2025年底发射至太阳同步低地球轨道。它还强调了小型任务在为学生和研究人员提供培训和领导力发展机会、推进大型望远镜技术方面的重要作用，并分享了来自学术界、政府和工业界合作伙伴合作中学到的经验教训。 显示英文摘要

The Star-Planet Activity Research CubeSat (SPARCS) is a NASA-funded 6U-CubeSat mission designed to monitor ultraviolet (UV) radiation from low-mass stars. These stars' relatively high-frequency and high-energy UV flares significantly affect the atmospheres of orbiting exoplanets, driving atmospheric loss and altering the conditions for habitability. SPARCS aims to capture time-resolved photometric data in the far-UV and near-UV simultaneously to better characterize the flares and detect the strongest and rarest among them. In addition, SPARCS is testing innovative technology, such as delta-doped detectors with near 100% internal quantum efficiency and detector-integrated metaldielectric UV bandpass filters. This mission will increase the technology readiness level of these critical components, positioning them for inclusion in future flagship missions like the Habitable Worlds Observatory. This paper outlines SPARCS' mission goals and provides an update as the spacecraft is completed and awaits its planned late-2025 launch to a sun-synchronous low-Earth orbit. It also highlights the critical role of small missions in providing training and leadership development opportunities for students and researchers, advancing technology for larger observatories, and shares lessons learned from collaborations between academic, government, and industry partners.

[30] arXiv:2507.03506 (交叉列表自 astro-ph.IM) [中文pdf, pdf, html, 其他]

标题： 巨行星高能粒子沉降的大气效应研究与HWO 显示英文标题

标题： Study of the atmospheric effects of energetic particle precipitations on giant planets with HWO

J-Y. Chaufray (1), W. Dunn (2), L.N. Fletcher (3), L. Fossati (4), M. Galand (5), L. Gkouvelis (6), C.M. Jackmann (7), L. Lamy (8,9), L. Roth (10) ((1) LATMOS-IPSL, UVSQ Paris Saclay, Sorbonne Université, CNRS, France,(2) MSSL, UCL, Dorking, UK, (3) SPA, University of Leicester, Leicester, UK, (4) IWF, OeAW, Graz, Austria, (5) Imperial College, London, UK, (6) LMU, University Observatory, Munich, Germany, (7) Astronomy and Astrophysics Section, Dublin Institute for Advanced Studies (DIAS), Dunsink Observatory, Dublin, Ireland, (8) LAM, Marseille, France, (9) LIRA, Meudon, France, (10) SPP, KTH, Stockholm, Sweden)

评论： 会议 “迈向宜居世界观测站：远见科学与变革性技术，2025年7月28日 - 2025年7月31日”

主题： 天体物理学的仪器与方法 (astro-ph.IM) ; 地球与行星天体物理学 (astro-ph.EP)

紫外极光发射来自巨行星，是由外部大气的高能粒子与大气相互作用产生的。它们已经在木星、土星和天王星上被观测到，应该也存在于海王星上。即使这些机制相似，由于每个行星特有的磁层等离子体来源以及磁层的结构和动力学，每个行星都是独特的。这些沉降如何在局部和全球大气尺度上改变大气加热、动力学和化学平衡仍然知之甚少，尤其是在天王星和海王星上，这对于理解巨行星和系外行星的全球大气-磁层系统至关重要。在本文中，我们介绍了未来由搭载在\textit{宜居世界观测站} (HWO) 上的仪器进行的观测将如何提供新的信息，以更好地理解这些沉降的起源及其大气效应。一个主要的兴趣点是天王星和海王星遥远的磁层，这些磁层尚未被轨道航天器探索，其紫外极光发射仍处于（天王星）或低于（海王星）哈勃太空望远镜的灵敏度。\textit{波卢克斯}是一种这样的紫外仪器概念，它将在精细的空间尺度上实现前所未有的高光谱分辨率，并进行极化观测，而\textit{LUMOS}，另一个紫外仪器将用良好的光谱分辨率成像整个极光区域。 显示英文摘要

UV auroral emissions from giant planets are produced by extra-atmospheric energetic particles interacting with an atmosphere. They have been observed on Jupiter, Saturn and Uranus and should be present on Neptune. Even if the mechanisms are similar, each planet is unique due to its specific source of magnetospheric plasma and the structure and dynamics of its magnetosphere. How these precipitations modify atmospheric heating, dynamics and chemical balance at local and global atmospheric scale is still poorly known, especially on Uranus and Neptune, and critical to understanding the global atmosphere-magnetosphere system of giant planets and exoplanets. In this manucript we present how future observations by instruments, aboard \textit{the Habitable World Observatory} (HWO) will provide new information to better understand the origin and the atmospheric effects of these precipitations. A major interest is for the distant magnetospheres of Uranus and Neptune, never explored by an orbital spacecraft whose UV auroral emissions remains at (Uranus) or below (Neptune) the HST sensitivity. \textit{Pollux} is one such UV instrument concept, which will enable unprecedented high spectral resolution at fine spatial scale not previously seen and polarimetric observations of the planetary aurorae while \textit{LUMOS}, another UV instrument will image the full auroral regions with a good spectral resolution.

[31] arXiv:2507.03679 (交叉列表自 astro-ph.GA) [中文pdf, pdf, html, 其他]

标题： JWST 预期在猎户座星云团中的棕矮星候选体光谱 显示英文标题

标题： JWST Spectra of Brown Dwarf Candidates in the Orion Nebula Cluster

K. L. Luhman

评论： MNRAS快报，待发表

主题： 星系的天体物理学 (astro-ph.GA) ; 地球与行星天体物理学 (astro-ph.EP)

我分析了200个朝向猎户座星云团（ONC）的天体的档案光谱，这些光谱是由詹姆斯·韦布空间望远镜（JWST）上的近红外光谱仪（NIRSpec）获得的。 我利用这些数据来评估星团成员身份并测量目标的光谱类型。 53个天体被归类为可能的星团成员，其中24个的光谱类型表明可能是棕矮星（$>$M6）。 NIRSpec的目标中有7个之前被识别为“木星质量双星天体”（JuMBOs），但根据NIRSpec的数据，它们都是背景天体而非棕矮星。 这些天体的光谱分类与我最近对ONC中JWST测光的研究结果一致，该研究发现只有少数JuMBO组分具有棕矮星预期的颜色，其中没有一个形成具有独特宽分离度或相对于已知棕矮星双星而言低质量的双星。 显示英文摘要

I present an analysis of archival spectra of 200 sources toward the Orion Nebula Cluster (ONC) that were obtained with the Near-Infrared Spectrograph (NIRSpec) on board the James Webb Space Telescope (JWST). I have used these data to assess cluster membership and measure spectral types for the targets. Fifty-three sources are classified as likely cluster members, 24 of which have spectral types that are suggestive of brown dwarfs ($>$M6). Seven of the NIRSpec targets were previously identified as "Jupiter-mass binary objects" (JuMBOs), all of which are background sources rather than brown dwarfs based on the NIRSpec data. The spectral classifications of those objects are consistent with the results of my recent study of the JWST photometry in the ONC, which found that only a few JuMBO components have the colors expected for brown dwarfs, none of which form pairs that have uniquely wide separations or low masses relative to known binary brown dwarfs.

[32] arXiv:2507.04066 (交叉列表自 astro-ph.SR) [中文pdf, pdf, html, 其他]

标题： 由APOGEE观测的开普勒、K2和TESS中M型矮星行星宿主恒星的金属量：与系外行星半径和轨道周期的趋势 显示英文标题

标题： Metallicities of M Dwarf Planet Host Stars from Kepler, K2, and TESS observed by APOGEE: Trends with Exoplanetary Radii and Orbital Periods

Fábio Wanderley, Katia Cunha, Diogo Souto, Verne Smith, Simone Daflon

评论： 已被《天文学杂志》（AJ）接受发表

主题： 太阳与恒星天体物理学 (astro-ph.SR) ; 地球与行星天体物理学 (astro-ph.EP)

研究系外行星种群的一个重要特性是宿主恒星金属量([M/H])。在本研究中，我们利用SDSS APOGEE调查的近红外高分辨率光谱和LTE计算的合成光谱，推导出45颗M型矮星（包含65颗系外行星）的恒星金属量和氧丰度。我们还研究了246颗围绕188颗M型矮星运行的系外行星的半径分布。获得的[M/H]与[O/M]分布表明，我们的样本主要由薄盘恒星组成，它们遵循银河系薄盘低-alpha序列的行为。发现半径小于3R$_{\oplus}$的小行星围绕金属量范围为(-0.6$<$[M/H]$<$+0.3)的恒星运行，而样本中的大行星仅围绕[M/H]$>=0.0$的恒星运行。这些结果表明，虽然小行星可以在不同环境中形成，但大行星更倾向于在金属丰富的原行星盘中形成。轨道周期P$_{\rm orb}<$4.3天的系外行星平均而言围绕比轨道周期更长的行星金属量更高的恒星。这个阈值小于FGK恒星（8-10天）发现的阈值，可能与M型矮星具有较小的尘埃蒸发半径有关。半径R$_{\rm p}>$4R$_{\oplus}$的系外行星的分布显示在轨道周期2到5天之间有集中现象，这可能是向内轨道迁移的结果。单次检测到的系外行星和多行星系统中的行星之间也表现出不同的行为，后者平均围绕金属量更低的恒星运行，且轨道周期大致不超过3天。 显示英文摘要

One important property in studying the exoplanet population is the host star metallicity ([M/H]). In this study, we derived stellar metallicities and oxygen abundances for 45 M dwarf stars (with 65 exoplanets) using the near-infrared high-resolution spectra from the SDSS APOGEE survey and synthetic spectra computed in LTE. We also investigated the exoplanetary radii distribution for a larger sample of 246 exoplanets orbiting 188 M dwarf stars. The [M/H] versus [O/M] distribution obtained indicates that our sample is composed mainly of thin disk stars, which follow the behavior of the low-alpha sequence in the Milky Way thin disk. Small planets with radii smaller than 3R$_{\oplus}$ were found around stars with a range of metallicities (-0.6$<$[M/H]$<$+0.3), while larger planets of the sample orbit only stars with [M/H]$>=0.0$. These results indicate that while small planets can form in different environments, larger planets preferentially form in metal-rich protoplanetary disks. Exoplanets with P$_{\rm orb}<$4.3 days orbit on average more metal-rich stars than planets with longer periods. This threshold is smaller than that found for FGK stars (8--10 days) and might be related to M dwarfs having a smaller dust sublimation radius. The distribution of exoplanets with R$_{\rm p}>$4R$_{\oplus}$ shows a concentration at orbital periods between 2 and 5 days, which may result from inward orbital migration. There is also a different behavior between single-detected exoplanets and planets from multiplanetary systems, with the latter being found on average around more metal-poor stars, and with orbital periods roughly up to 3 days.

替换提交 (展示 9 之 9 条目 )

[33] arXiv:2503.18128 (替换) [中文pdf, pdf, 其他]

标题： 彗星荧光模型用于氰化物的$ν_3$振动带 显示英文标题

标题： A cometary Fluorescence Model for the $ν_3$ Vibrational Band of Cyanogen

P. Hardy, P. Rousselot, C. Richard, V. Boudon, X. Landsheere, A. Voute, L. Manceron, F. Kwabia Tchana

主题： 地球与行星天体物理学 (astro-ph.EP)

氰化物（$\mathrm{C_2N_2}$）长期以来被认为存在于彗星中，并有助于CN自由基的形成。 到目前为止，地面设施的观测尚未成功检测到该物质，但罗塞塔任务通过ROSINA质谱仪的原位观测，在67P/丘留莫夫-杰里科夫斯基彗星的彗发中检测到了该物质。 为了研究其他彗星中红外光谱中的存在，我们开发了$\nu_3$基本带的荧光模型。 从氰化物的新实验室高分辨率红外光谱中，我们分析了$\mathrm{C_2N_2}$的$\nu_3$带区域，中心位于4.63$\mu m$（2158$\mathrm{cm^{-1}}$）。 除了线位置和强度外，还获得了基态和激发振动态的分子参数。 这些参数使我们能够为氰化物开发一个荧光模型。 给出了彗星彗发中氰化物$\nu_3$带的逐线激发率。 讨论了彗星C/2022 E3（ZTF）光谱中氰化物的丰度上限。 显示英文摘要

Cyanogen ($\mathrm{C_2N_2}$) is suspected for a long time to be present in comets and to contribute to the creation of the CN radical. So far no observations with ground-based facilities have managed to detect this species but the Rosetta mission, thanks to in situ observations with the ROSINA mass spectrometer detected this species in the coma of 67P/Churyumov-Gerasimenko. To investigate its presence from infrared spectra in other comets, we developed a fluorescence model for the $\nu_3$ fundamental band. From new laboratory high-resolution infrared spectra of cyanogen, we analyzed the region of the $\nu_3$ band of $\mathrm{C_2N_2}$, centered around 4.63 $\mu m$ (2158 $\mathrm{cm^{-1}}$). In addition to line positions and intensities, molecular parameters for the ground and excited vibrational state were obtained. These parameters allowed us to develop a fluorescence model for cyanogen. Line-by-line excitation rates of the $\nu_3$ band of cyanogen in cometary comae are presented. An upper limit of the abundance of cyanogen in a spectrum of comet C/2022 E3 (ZTF) is discussed.

[34] arXiv:2503.21702 (替换) [中文pdf, pdf, html, 其他]

标题： 用高斯过程实现鲁棒的系外行星大气反演 显示英文标题

标题： Enabling Robust Exoplanet Atmospheric Retrievals with Gaussian Processes

Yoav Rotman, Luis Welbanks, Michael R. Line, Peter McGill, Michael Radica, Matthew C. Nixon

评论： 被ApJ接收，22页，8图

主题： 地球与行星天体物理学 (astro-ph.EP) ; 天体物理学的仪器与方法 (astro-ph.IM)

大气反演是解释系外行星透射和掩食光谱的重要工具，能够对行星大气的化学成分、气溶胶特性及热结构进行定量约束。 詹姆斯·韦布空间望远镜（JWST）提供了前所未有的光谱精度、分辨率和波长覆盖范围，为行星系统的形成、演化、气候和潜在可居住性提供了变革性的见解。 然而，这一机遇伴随着挑战：建模假设和未考虑的噪声或信号源可能会导致反演结果及其解释产生偏差。 为解决这些限制，我们引入了一种由高斯过程（GP）辅助的大气反演框架，该框架能够灵活地考虑系外行星光谱中未建模的特征和相关噪声。 我们在合成的JWST观测数据上验证了该方法，并表明GP辅助的反演方法在推导的丰度中减少了偏差，并比传统方法更好地捕捉模型与数据之间的不匹配。 我们还引入了均方误差的概念，以量化偏差和方差之间的权衡，认为该指标比单独的偏差更能准确反映反演性能。 随后，我们重新分析了JWST的NIRISS/SOSS透射光谱WASP-96 b，发现GP辅助的反演方法对CO2和H2O给出了更宽的约束，可能缓解之前反演结果与平衡预测之间的矛盾。 我们的GP框架在提供精确和准确的约束的同时，也突出了模型无法解释数据的区域。 随着JWST的发展和未来设施的投入使用，对数据和模型局限性的深入理解将变得至关重要，而像本文提出的这种GP增强的反演方法提供了一条有原则的前进路径。 显示英文摘要

Atmospheric retrievals are essential tools for interpreting exoplanet transmission and eclipse spectra, enabling quantitative constraints on the chemical composition, aerosol properties, and thermal structure of planetary atmospheres. The James Webb Space Telescope (JWST) offers unprecedented spectral precision, resolution, and wavelength coverage, unlocking transformative insights into the formation, evolution, climate, and potential habitability of planetary systems. However, this opportunity is accompanied by challenges: modeling assumptions and unaccounted-for noise or signal sources can bias retrieval outcomes and their interpretation. To address these limitations, we introduce a Gaussian Process (GP)-aided atmospheric retrieval framework that flexibly accounts for unmodeled features and correlated noise in exoplanet spectra. We validate this method on synthetic JWST observations and show that GP-aided retrievals reduce bias in inferred abundances and better capture model-data mismatches than traditional approaches. We also introduce the concept of mean squared error to quantify the trade-off between bias and variance, arguing that this metric more accurately reflects retrieval performance than bias alone. We then reanalyze the NIRISS/SOSS JWST transmission spectrum of WASP-96 b, finding that GP-aided retrievals yield broader constraints on CO2 and H2O, possibly alleviating tension between previous retrieval results and equilibrium predictions. Our GP framework provides precise and accurate constraints while highlighting regions where models fail to explain the data. As JWST matures and future facilities come online, a deeper understanding of the limitations of both data and models will be essential, and GP-enabled retrievals like the one presented here offer a principled path forward.

[35] arXiv:2506.06433 (替换) [中文pdf, pdf, html, 其他]

标题： 哈罗6-13致密嵌入原行星盘中的大型旋臂结构 显示英文标题

标题： Grand Design Spiral Arms in the Compact, Embedded Protoplanetary Disk of Haro 6-13

Jane Huang, Masataka Aizawa, Jaehan Bae, Sean M. Andrews, Myriam Benisty, Edwin A. Bergin, Stefano Facchini, Christian Ginski, Michael Küffmeier

评论： 被ApJ接受

主题： 地球与行星天体物理学 (astro-ph.EP) ; 太阳与恒星天体物理学 (astro-ph.SR)

毫米波连续谱螺旋臂迄今为止仅在少数原行星盘中被检测到，因此我们对它们形成时的条件了解有限。 特别是与大盘相比，小盘（$R\lessapprox 50$au）中的子结构尚未得到很好的表征。 我们展示了围绕T星系恒星Haro 6-13的盘在1.3毫米连续谱的ALMA观测结果，分辨率为$\sim0.04''$（$\sim5$au）。 在盘半径从$\sim10-35$au处检测到一对低对比度的螺旋臂。 它们可以近似为阿基米德螺旋，其倾角范围从$\sim10-30^\circ$。 在1.3毫米和3毫米之间的盘平均光谱指数（$\alpha=2.1$）较低，以及高亮度温度表明，毫米波连续谱可能是光学厚的，因此可能隐藏了足够的质量使盘变得引力不稳定并形成螺旋臂。 CO观测显示，Haro 6-13被包层包围，这提出了吸积可能有助于螺旋臂形成的可能性。 显示英文摘要

Millimeter continuum spiral arms have so far only been detected in a handful of protoplanetary disks, and thus we have a limited understanding of the circumstances in which they can form. In particular, substructures in small disks ($R\lessapprox 50$ au) have not been well-characterized in comparison with large disks. We present ALMA 1.3 mm continuum observations of the disk around the T Tauri star Haro 6-13 at a resolution of $\sim0.04''$ ($\sim5$ au). A pair of low-contrast spiral arms are detected at disk radii from $\sim10-35$ au. They can be approximated as Archimedean spirals with pitch angles ranging from $\sim10-30^\circ$. The low value of the disk-averaged spectral index between 1.3 and 3 mm ($\alpha=2.1$) and the high brightness temperatures suggest that the millimeter continuum is likely optically thick and thus may hide sufficient mass for the disk to become gravitationally unstable and form spiral arms. CO observations have shown that Haro 6-13 is surrounded by an envelope, raising the possibility that infall is facilitating spiral arm formation.

[36] arXiv:2506.16063 (替换) [中文pdf, pdf, html, 其他]

标题： （再）定义行星——行星的基本平面 显示英文标题

标题： (Re)-Defining Planets -- the Fundamental Plane of Planets

Madhu Kashyap Jagadeesh, Arkil D. Parikh, Margarita Safonova, Bernard Foing

评论： 8页，7图 提交至MNRAS

主题： 地球与行星天体物理学 (astro-ph.EP) ; 天体物理学的仪器与方法 (astro-ph.IM)

6000多个系外行星现在通过各种技术被探测到，据估计仅在我们的银河系中就有数十亿颗行星。 它们被称为超级地球、热地球、迷你海王星、热海王星、次海王星、土星、木星、热木星、气体巨行星、冰巨行星、岩石行星、类地行星、次地行星、超级类地行星等等。 这促使了许多关于系外行星分类的近期研究工作。 然而，目前仍然没有对“什么是行星？”的基本定义。 IAU在2006年提出了一种定义，但该定义引发了比解决更多问题。 在这里的第一个雄心勃勃的任务是确定行星尺寸/质量的限制。 下限可以假设为米玛斯的质量——大约达到近似球形流体静力平衡形状所需的最小质量。 上限可能更容易——对于构成恒星的物体有一个自然的下限： ~0.08 SU。 但随后有棕矮星：IAU将棕矮星定义为超过氘燃烧极限（~13 JU）的天体，而巨大的系外行星通常具有~0.3至~60 JU的质量。 解决这个问题需要汇集定义行星的定量基本物理参数。 质量和半径是两个基本属性，我们建议使用第三个相关参数：转动惯量。 基于此，我们创建了基本的行星平面，其中两个参数与第三个参数相关，类似于基本的银河平面。 首次在本工作中构建了带有转折点图的的基本行星平面。 我们定义行星为“一个围绕恒星或不受约束的天体，位于基本行星平面上，在质量范围0.02 EU到13 JU之间”。 显示英文摘要

6000+ exoplanets are now detected using various techniques, with estimates of billions of planets existing in our Galaxy alone. They are called super-Earths, hot Earths, mini-Neptunes, hot Neptunes, sub-Neptunes, Saturns, Jupiters, hot Jupiters, gas giants, ice giants, rocky, terran, subterran, superterran, and so on. This prompted the emergence of many recent works on taxonomy, or classification, of exoplanets. However, there is still no basic, fundamental definition of 'What is a planet?'. IAU has forwarded a definition in 2006 which, however, raised more questions than it solved. The first ambitious task here is to establish if there are limits on the size/mass of planets. The lower mass limit may be assumed as of Mimas - approximately minimum mass required to attain a nearly spherical hydrostatic equilibrium shape. The upper mass limit may be easier - there is a natural lower limit to what constitutes a star: ~0.08 SU. But then there are brown dwarfs: IAU has defined brown dwarfs as objects that exceed the deuterium burning limit (~13 JU), and giant exoplanets generally have masses of ~0.3 to ~60 JU. The resolution requires assembling the basic physical parameters that define planets quantitatively. Mass and radius are the two fundamental properties, and we propose to use a third correlated parameter: the moment of inertia. Based on this, we create the fundamental planet plane where the two parameters are correlated with the third, similar to a fundamental galactic plane. The fundamental planetary plane with turn-off point diagrams is constructed for the first time in this work. We define a planet as 'A celestial spherical object, bound to a star or unbound, that lies on the fundamental planetary plane, within a mass range between 0.02 EU to 13 JU'.

[37] arXiv:2506.16481 (替换) [中文pdf, pdf, html, 其他]

标题： CQ Tau和MWC 758周围动态扰动的原行星盘中的SO发射 显示英文标题

标题： SO emission in the dynamically perturbed protoplanetary disks around CQ Tau and MWC 758

Francesco Zagaria, Haochang Jiang, Gianni Cataldi, Stefano Facchini, Myriam Benisty, Yuri Aikawa, Sean Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Pietro Curone, Ian Czekala, Daniele Fasano, Cassandra Hall, Iain Hammond, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Jensen Lawrence, Giuseppe Lodato, François Ménard, Christophe Pinte, Giovanni P. Rosotti, Jochen Stadler, Richard Teague, Leonardo Testi, David Wilner, Andrew Winter, Tomohiro Yoshida

评论： 已接受发表于ApJ。23页 7图

主题： 地球与行星天体物理学 (astro-ph.EP)

我们报告在档案中的阿塔卡马大型毫米波/亚毫米波阵列(ALMA)观测中意外检测到围绕CQ Tau的螺旋状原行星盘（具有$\approx4.9\sigma$显著性）和MWC 758（具有$\approx3.4\sigma$显著性）中的SO$J_N=6_5-5_4$（219.949 GHz）旋转跃迁。 在前者中，SO辐射呈环状，来源于连续谱空腔的边缘，并在目前可用的光谱分辨率下定性上与开普勒旋转一致。 而在后者中，虽然SO辐射主要来自连续谱空腔内部，但也延伸到连续谱环，其形态和动力学不太清晰。 我们将这些源置于其他已报道SO检测的原行星盘的背景下，并讨论SO可能的起源，即（热）解吸或气相中的形成。 我们认为这些过程可能由未被观测到的嵌入式大质量伴星、阴影或晚期吸积引起的动态扰动所促进，从而暗示了扰动的动力学与（这些）原行星盘中SO辐射之间可能存在联系。 如果得到证实，我们的解释将意味着这些系统中的化学演化时间尺度可能比通常假设的要短得多，表明动态扰动可能通过改变其形成环境的挥发物组成来影响新生（原）行星的成分。 显示英文摘要

We report the serendipitous detection of the SO $J_N=6_5-5_4$ (219.949 GHz) rotational transition in archival Atacama Large Millimeter/submillimeter Array (ALMA) observations of the spiral hosting protoplanetary disks around CQ Tau (with $\approx4.9\sigma$ significance) and MWC 758 (with $\approx3.4\sigma$ significance). In the former, the SO emission comes in the shape of a ring, arises from the edge of the continuum cavity, and is qualitatively consistent, at the currently available spectral resolution, with being in Keplerian rotation. In the latter, instead, while arising primarily from inside the continuum cavity, the SO emission also extends to the continuum ring(s), and its morphology and kinematics are less clear. We put these sources in the context of the other protoplanetary disks where SO detections have been previously reported in the literature and discuss the possible origins of SO in terms of (thermal) desorption or formation in the gas phase. We argue that these processes might be fostered by dynamical perturbations caused by unseen embedded massive companions, shadows, or late-time infall, thus suggesting a possible link between perturbed dynamics and SO emission in (these) protoplanetary disks. If confirmed, our interpretation would imply that chemical evolution timescales could be significantly shorter in these systems than is commonly assumed, indicating that dynamical perturbations might influence the composition of newborn (proto-)planets by altering the volatile makeup of their formation environment.

[38] arXiv:2506.20919 (替换) [中文pdf, pdf, html, 其他]

标题： HD 23514周围巨大撞击盘中挥发性气体的发现 显示英文标题

标题： Discovery of Volatile Gas in the Giant Impact Disk around the 150-Myr old HD 23514

Kate Y. L. Su, Attila Moór, Chengyan Xie, Ilaria Pascucci, George H. Rieke, Ágnes Kóspál, Mark C. Wyatt, Péter Ábrahám, Luca Matrà, Zoe Roumeliotis, D. J. Wilner

评论： 已接受发表于ApJL；修正了拼写错误；更新了DOI

主题： 地球与行星天体物理学 (astro-ph.EP) ; 太阳与恒星天体物理学 (astro-ph.SR)

我们报告在HD 23514周围发现了CO$_2$气体发射，HD 23514是$\sim$1.5亿年古老的毕宿星团中的一个F5V恒星，该恒星拥有一个罕见的巨撞击盘，其独特的矿物学由石英尘埃主导。 我们表明，尘埃特征在数十年内保持稳定，并且产生$\sim$9$\mu$米特征的亚$\mu$米颗粒与恒星亚天文单位范围内的热CO$_2$分子共空间分布。 检查15年前拍摄的斯皮策光谱，我们表明CO$_2$发射在4.3$\sigma$显著性下也存在。 存在微小的二氧化硅颗粒和易挥发气体需要特殊条件以防止由于恒星辐射压力和光致解离引起的快速损失。 我们探讨了几种解释观测特性的途径，并认为过去的大规模撞击和/或剥离大气事件，涉及含有类似碳质球粒陨石物质的挥发性内容的大天体，可以同时解释二氧化硅和挥发性发射。 我们的发现为新形成行星或早期太阳系演化过程中巨大撞击阶段中行星esimal可能保留的挥发物量提供了重要的背景。 显示英文摘要

We report the discovery of CO$_2$ gas emission around HD 23514, an F5V star in the $\sim$150 Myr-old Pleiades cluster, hosting one of the rare giant-impact disks with unique mineralogy dominated by silica dust. We show that the dust feature remains stable over several decades, and that the sub-$\mu$m grains, which give rise to the $\sim$9 $\mu$m feature, are co-spatial with the hot CO$_2$ molecules within the sub-au vicinity of the star. Examining the Spitzer spectrum taken 15 years earlier, we show that the CO$_2$ emission was also present at 4.3 $\sigma$ significance. The existence of tiny silica grains and volatile gas requires special conditions to prevent the rapid loss caused by stellar radiation pressure and photodissociation. We explore several pathways explaining the observed properties and suggest that a past giant impact and/or stripping atmospheric event, involving large bodies with volatile content similar to the carbonaceous chondritic material, can simultaneously explain both the silica and volatile emission. Our discovery provides an important context for the amount of volatiles that a newly formed planet or the largest planetesimals could retain during the giant impact phase in the early solar system evolution.

[39] arXiv:2507.02757 (替换) [中文pdf, pdf, html, 其他]

标题： 发现和初步表征第三个星际物体：3I/ATLAS 显示英文标题

标题： Discovery and Preliminary Characterization of a Third Interstellar Object: 3I/ATLAS

Darryl Z. Seligman, Marco Micheli, Davide Farnocchia, Larry Denneau, John W. Noonan, Henry H. Hsieh, Toni Santana-Ros, John Tonry, Katie Auchettl, Luca Conversi, Maxime Devogèle, Laura Faggioli, Adina D. Feinstein, Marco Fenucci, Marin Ferrais, Tessa Frincke, Olivier R. Hainaut, Kyle Hart, Andrew Hoffman, Carrie E. Holt, Willem B. Hoogendam, Mark E. Huber, Emmanuel Jehin, Theodore Kareta, Jacqueline V. Keane, Michael S. P. Kelley, Tim Lister, Kathleen Mandt, Dušan Marčeta, Karen J. Meech, Mohamed Amine Miftah, Marvin Morgan, Francisco Ocaña, Eloy Peña-Asensio, Benjamin J. Shappee, Robert J. Siverd, Aster G. Taylor, Michael A. Tucker, Richard Wainscoat, Robert Weryk, James J. Wray, Atsuhiro Yaginuma, Bin Yang, Quanzhi Ye, Qicheng Zhang

评论： 提交至AAS期刊。13页，8图，1表。社区后续组织可在此处找到：https://3i-atlas.github.io/ 该论文的showyourwork!版本可在此处找到：https://github.com/3I-ATLAS/discovery-paper

主题： 地球与行星天体物理学 (astro-ph.EP) ; 星系的天体物理学 (astro-ph.GA) ; 天体物理学的仪器与方法 (astro-ph.IM)

我们报告初步观察结果，旨在表征第三个星际物体候选者。 该物体3I/ATLAS或C/2025 N1（ATLAS）于2025年7月1日世界时被发现，其轨道偏心率为$e\sim6.1$，近日点为$q\sim 1.36$天文单位，倾角为$\sim175^\circ$，以及双曲线速度为$V_\infty\sim 58$公里每秒$^{-1}$。 我们报告使用加拿大-法国-夏威夷望远镜和甚大望远镜获得的深度叠加图像，这些图像解析出了一个紧凑的彗发。 使用来自多个较小地面望远镜的图像，我们在$\sim4$天的时间跨度内发现该物体的光变曲线变化最小。 该物体的可见/近红外光谱斜率为17.1$\pm$0.2%/100纳米，与其他星际物体以及原始太阳系小天体（彗星和D型小行星）相当，尽管这一结果可能受到彗发污染的影响。 3I/ATLAS将在2025年9月初之前可观测，然后由于太阳张角较低，在近日点附近将无法被地球上的观测站观测到。 它将在2025年11月下旬再次从地面上可观测。 尽管这种限制不幸地禁止了在3I/ATLAS活动可能达到峰值的近日点进行详细的地球观测，但火星上的航天器可以在此时进行有价值的观测。 鼓励通过地面和空间望远镜，以及可能位于火星上的航天器对3I/ATLAS进行额外的测光、光谱和偏振监测，以表征3I/ATLAS的自转光变曲线、活动演化、非引力加速度以及形成条件的组成指标。 显示英文摘要

We report initial observations aimed at the characterization of a third interstellar object candidate. This object, 3I/ATLAS or C/2025 N1 (ATLAS), was discovered on 2025 July 1 UT and has an orbital eccentricity of $e\sim6.1$, perihelion of $q\sim 1.36$ au, inclination of $\sim175^\circ$, and hyperbolic velocity of $V_\infty\sim 58$ km s$^{-1}$. We report deep stacked images obtained using the Canada-France-Hawaii Telescope and the Very Large Telescope that resolve a compact coma. Using images obtained from several smaller ground-based telescopes, we find minimal light curve variation for the object over a $\sim4$ day time span. The visible/near-infrared spectral slope of the object is 17.1$\pm$0.2 %/100 nm, comparable to other interstellar objects and primitive solar system small bodies (comets and D-type asteroids), although this result is likely affected by some coma contamination. 3I/ATLAS will be observable through early September 2025, then unobservable by Earth-based observatories near perihelion due to low solar elongation. It will be observable again from the ground in late November 2025. Although this limitation unfortunately prohibits detailed Earth-based observations at perihelion when the activity of 3I/ATLAS is likely to peak, spacecraft at Mars could be used to make valuable observations at this time. Additional photometric, spectroscopic, and polarimetric monitoring of 3I/ATLAS by ground- and space-based telescopes, and possibly spacecraft based at Mars, are highly encouraged for characterizing 3I/ATLAS's rotational light curve, activity evolution, nongravitational acceleration, and compositional indicators of formation conditions.

[40] arXiv:2505.14712 (替换) [中文pdf, pdf, html, 其他]

标题： 李群理论在多极矩与旋转流体静止体形状中的应用 显示英文标题

标题： Lie Group Theory of Multipole Moments and Shape of Stationary Rotating Fluid Bodies

Sergei M. Kopeikin (University of Missouri-Columbia, USA)

评论： 83页

主题： 经典物理 (physics.class-ph) ; 地球与行星天体物理学 (astro-ph.EP) ; 太阳与恒星天体物理学 (astro-ph.SR) ; 广义相对论与量子宇宙学 (gr-qc) ; 数学物理 (math-ph) ; 流体动力学 (physics.flu-dyn) ; 地球物理 (physics.geo-ph)

我们提出了一种严格框架，用于确定均匀旋转、自引力流体物体的平衡构型。 这项工作解决了建模天体如恒星和行星中的旋转变形的经典挑战。 通过将基础理论与现代数学工具相结合，我们开发了一个统一的形式，提高了天体物理背景下形状建模的精度和普遍性。 我们的方法将李群理论应用于矢量流，并使用诺伊曼级数求解函数方程。 我们通过李指数映射将克莱罗的经典线性微扰理论扩展到非线性领域，得到描述引力势和流体密度的非线性函数方程系统。 这些方程可以通过位移算子和诺伊曼级数求和进行解析处理，从而能够明确表征密度和引力扰动。 这导致了一个关于形状函数的精确非线性微分方程，描述了平衡变形，而无需假设缓慢旋转。 我们通过精确解验证了该框架，包括马克劳林椭球、雅可比椭球和单位指数多相体。 我们还引入了谱分解技术，用于分析径向调和函数和引力扰动。 利用维格纳的角动量加法形式，我们高效地计算了高阶非线性修正。 该框架包含了支持非线性洛夫数和引力多极矩推导的勒让德调和边界条件。 这项工作为建模天体物理和行星系统的旋转和潮汐变形提供了一个全面的非微扰方法。 显示英文摘要

We present a rigorous framework for determining the equilibrium configurations of uniformly rotating, self-gravitating fluid bodies. This work addresses the classical challenge of modeling rotational deformation in celestial objects such as stars and planets. By integrating foundational theory with modern mathematical tools, we develop a unified formalism that enhances the precision and generality of shape modeling in astrophysical contexts. Our method applies Lie group theory to vector flows and solves functional equations using the Neumann series. We extend Clairaut's classical linear perturbation theory into the nonlinear regime via Lie exponential mapping, yielding a system of nonlinear functional equations for gravitational potential and fluid density. These are analytically tractable using shift operators and Neumann series summation, enabling explicit characterization of density and gravitational perturbations. This leads to an exact nonlinear differential equation for the shape function, describing equilibrium deformation without assuming slow rotation. We validate the framework through exact solutions, including the Maclaurin spheroid, Jacobi ellipsoid, and unit-index polytrope. We also introduce spectral decomposition techniques for analyzing radial harmonics and gravitational perturbations. Using Wigner's formalism for angular momentum addition, we compute higher-order nonlinear corrections efficiently. The framework includes boundary conditions for Legendre harmonics, supporting the derivation of nonlinear Love numbers and gravitational multipole moments. This work offers a comprehensive, non-perturbative approach to modeling rotational and tidal deformations in astrophysical and planetary systems.

[41] arXiv:2505.24560 (替换) [中文pdf, pdf, html, 其他]

标题： 基准棕矮星——I。 一个蓝色M2 + T5宽双星和一个可能年轻的[M4 + M4] + [T7 + T8]分级四重星 显示英文标题

标题： Benchmark brown dwarfs -- I. A blue M2 + T5 wide binary and a probable young [M4 + M4] + [T7 + T8] hierarchical quadruple

Z. H. Zhang, F. Navarete, M. C. Galvez-Ortiz, H. R. A. Jones, A. J. Burgasser, P. Cruz, F. Marocco, N. Lodieu, Y. Shan, B. Gauza, R. Raddi, M. R. Huang, R. L. Smart, S. Baig, G. Cheng, D. J. Pinfield

评论： 13页，10图

主题： 太阳与恒星天体物理学 (astro-ph.SR) ; 地球与行星天体物理学 (astro-ph.EP)

基准褐矮星在宽双星系统中对于表征亚恒星天体和校准大气和演化模型至关重要。 然而，具有低于太阳金属量、非常低温或适合动态质量测量的褐矮星基准非常稀少，这限制了我们在整个质量、年龄和金属量范围内的理解。 我们介绍了通过使用CatWISE2020和Gaia目录进行有针对性的搜索而发现的两个包含T型矮星伴星的新多重系统。 L 122-88 AB是一个宽双星系统，由一颗轻微金属贫乏的M2型矮星和一颗T5型矮星组成，距离为33.106+/-0.014 pc，两者相距215.6角秒。 对L 122-88 A的近红外光谱进行大气模型拟合表明其具有轻微金属贫乏的成分([Fe/H] = -0.2)。 UPM J1040-3551 AB是一个候选的分级四重系统，距离为25.283+/-0.013 pc，由两个M4型矮星的可能天体测量双星和一个可能未分辨的光谱双星（T7和T8型矮星）组成，与主星相距65.48角秒。 在UPM J1040-3551 A中检测到的H-alpha发射表明其年龄范围为0.3-2.0 Gyr。 这个年龄估计表明T8型成分的质量在9到28倍木星质量之间，可能将其归类为行星质量物体。 这些系统增加了基准褐矮星的样本，特别是在低温这一研究不足的领域，为改进我们对亚恒星天体的理解提供了宝贵的机会。 显示英文摘要

Benchmark brown dwarfs in wide binary systems are crucial for characterizing substellar objects and calibrating atmospheric and evolutionary models. However, brown dwarf benchmarks with subsolar metallicity, very cool temperatures, or suitability for dynamical mass measurements are rare, limiting our understanding across the full range of mass, age, and metallicity. We present the discovery of two new multiple systems containing T dwarf companions, identified through a targeted search using CatWISE2020 and Gaia catalogues. L 122-88 AB is a wide binary comprising a mildly metal-poor M2 dwarf and a T5 dwarf, separated by 215.6 arcsec at a distance of 33.106+/-0.014 pc. Atmospheric model fitting to the near infrared spectrum of L 122-88 A suggests a mildly metal-poor composition ([Fe/H] = -0.2). UPM J1040-3551 AB is a candidate hierarchical quadruple system at 25.283+/-0.013 pc, consisting of a likely astrometric binary of two M4 dwarfs and a probable unresolved spectral binary of T7 and T8 dwarfs, separated by 65.48 arcsec from the primary. The H-alpha emission detected in UPM J1040-3551 A indicates an age range of 0.3-2.0 Gyr. This age estimate suggests that the T8 component has a mass between 9 and 28 Jupiter masses, potentially classifying it as a planetary-mass object. These systems augment the sample of benchmark brown dwarfs, particularly in the underexplored regime of cool temperature, providing valuable opportunities for refining our understanding of substellar objects.