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Updated Catalog of Kepler Planet Candidates: Focus on Accuracy and Orbital Periods 开普勒候选行星更新目录:关注精度和轨道周期
Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-06-27 DOI: 10.3847/psj/ad0e6e
Jack J. Lissauer, Jason F. Rowe, Daniel Jontof-Hutter, Daniel C. Fabrycky, Eric B. Ford, Darin Ragozzine, Jason H. Steffen and Kadri M. Nizam
We present a new catalog of Kepler planet candidates that prioritizes accuracy of planetary dispositions and properties over uniformity. This catalog contains 4376 transiting planet candidates, including 1791 residing within 709 multiplanet systems, and provides the best parameters available for a large sample of Kepler planet candidates. We also provide a second set of stellar and planetary properties for transiting candidates that are uniformly derived for use in occurrence rate studies. Estimates of orbital periods have been improved, but as in previous catalogs, our tabulated values for period uncertainties do not fully account for transit timing variations (TTVs). We show that many planets are likely to have TTVs with long periodicities caused by various processes, including orbital precession, and that such TTVs imply that ephemerides of Kepler planets are not as accurate on multidecadal timescales as predicted by the small formal errors (typically 1 part in 106 and rarely >10−5) in the planets’ measured mean orbital periods during the Kepler epoch. Analysis of normalized transit durations implies that eccentricities of planets are anticorrelated with the number of companion transiting planets. Our primary catalog lists all known Kepler planet candidates that orbit and transit only one star; for completeness, we also provide an abbreviated listing of the properties of the two dozen nontransiting planets that have been identified around stars that host transiting planets discovered by Kepler.
我们提出了一个新的开普勒行星候选星表,它优先考虑行星布局和性质的准确性,而不是统一性。该星表包含 4376 颗凌日候选行星,其中 1791 颗位于 709 个多行星系统中,并为大量开普勒候选行星样本提供了最佳参数。我们还为凌日候选行星提供了第二套恒星和行星属性,这些属性是统一推导出来的,可用于发生率研究。对轨道周期的估计有所改进,但与以前的星表一样,我们表中的周期不确定值并没有完全考虑凌日时间变化(TTVs)。我们的研究表明,许多行星都可能有由各种过程(包括轨道前冲)引起的周期较长的凌日时间变化,这种凌日时间变化意味着开普勒行星的星历表在十几年的时间尺度上并不像开普勒纪期间测量的行星平均轨道周期的微小形式误差(通常为1/106,很少>10-5)所预测的那样精确。对归一化凌日持续时间的分析表明,行星的偏心率与伴星凌日行星的数量是反相关的。我们的主目录列出了所有已知的只围绕一颗恒星运行并凌日的开普勒候选行星;为了完整起见,我们还提供了一份简短的清单,列出了开普勒发现的凌日行星所在恒星周围已确定的二十多颗非凌日行星的特性。
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引用次数: 0
Using Hydrodynamic Similarity as a Verification Method for Impact Cratering Simulations in the FLAG Hydrocode 将水动力相似性作为 FLAG 水文编码中撞击塌陷模拟的验证方法
Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-06-19 DOI: 10.3847/psj/ad4bdb
Matthew C. Holmes, Wendy K. Caldwell, Joanne L. Budzien and Carl E. Johnson
Hydrodynamic codes (hydrocodes) are common tools for modeling hypervelocity impacts to provide insight into the physical phenomenon. Hydrocodes can simulate impacts from micrometer to kilometer spatial scales and reach impact velocities difficult to achieve in experimental settings. However, numerical models are approximations, and demonstrating that a numerical method is capable of providing physical results for these models is essential. In this work, we employ a hydrocode verification technique that leverages hydrodynamic similarity, a mathematical property of the conservation equations of fluid mechanics that form the basis for hydrocode models. Using the FLAG hydrocode, we simulate aluminum (Al) and basalt projectiles and targets at spatial scales spanning 7 orders of magnitude (hundreds of micrometers to kilometers). These materials were chosen because Al-6061 is a common material in spacecraft and satellites and basalt is a useful approximation of rocky astronomical bodies. Our results show that hydrodynamic similarity holds for each material model used and across spatial scales. We show that under certain conditions hydrodynamic similarity can apply in the presence of gravity and that similarity does not hold in the presence of strength models. We conclude that the FLAG hydrocode preserves important mathematical properties of fluid dynamics in hypervelocity impacts of Al-6061 and basalt.
流体动力学代码(水力代码)是模拟超高速撞击的常用工具,可帮助人们深入了解物理现象。水动力代码可以模拟从微米到千米空间尺度的撞击,并达到在实验环境中难以实现的撞击速度。然而,数值模型只是近似值,因此必须证明数值方法能够为这些模型提供物理结果。在这项工作中,我们利用流体力学相似性这一流体力学守恒方程的数学特性,采用了一种水力代码验证技术,该技术构成了水力代码模型的基础。我们使用 FLAG 水文编码模拟了铝(Al)和玄武岩射弹和目标,其空间尺度跨越 7 个数量级(从数百微米到数千米)。之所以选择这些材料,是因为铝-6061 是航天器和卫星中的常见材料,而玄武岩则是岩石天体的有用近似材料。我们的研究结果表明,流体力学相似性适用于所使用的每种材料模型和不同的空间尺度。我们的结果表明,在某些条件下,流体力学相似性可适用于存在重力的情况,而在存在强度模型的情况下,相似性则不成立。我们的结论是,FLAG 流体动力学代码保留了 Al-6061 和玄武岩超高速撞击中流体动力学的重要数学特性。
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引用次数: 0
Asteroid Impact Hazard Warning from the Near-Earth Object Surveyor Mission 近地天体探测器任务发出的小行星撞击危险警告
Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-06-19 DOI: 10.3847/psj/ad4d9e
Oliver Lay, Joe Masiero, Tommy Grav, Amy Mainzer, Frank Masci and Edward Wright
NASA's Near-Earth Object Surveyor mission, scheduled for launch in 2027 September, is designed to detect and characterize at least two-thirds of the potentially hazardous asteroids with diameters larger than 140 m in a nominal 5 yr mission. We describe a model to estimate the survey performance using a faster approach than the time domain survey simulator described in Mainzer et al. (2023). This model is applied to explain how the completeness for 5 and 10 yr surveys varies with orbit type and asteroid size and to identify orbits with notably high or low likelihoods of detection. Size alone is an incomplete proxy for impact hazard, so for each asteroid orbit, we also calculate the associated hazard based on the impact velocity and the relative likelihood of impact. We then estimate how effective the mission will be at anticipating impacts as a function of impact energy, finding that a 5 yr mission will identify 87% of potential impacts larger than 100 Mt (Torino-9, "Regional Devastation"). For a 10 yr mission, this increases to 94%. We also show how the distribution of warning time varies with impact energy.
美国国家航空航天局的近地天体勘测器任务计划于 2027 年 9 月发射,其目的是在名义上为期 5 年的任务中探测并描述至少三分之二直径大于 140 米的潜在危险小行星。我们描述了一个模型,该模型使用比 Mainzer 等人(2023 年)中描述的时域巡天模拟器更快的方法来估算巡天性能。该模型用于解释 5 年和 10 年勘测的完整性如何随轨道类型和小行星大小的变化而变化,并确定探测可能性明显较高或较低的轨道。单凭大小并不能完全代表撞击危险,因此对于每个小行星轨道,我们还根据撞击速度和撞击的相对可能性计算相关危险。然后,我们根据撞击能量的函数来估算任务在预测撞击方面的有效性,结果发现 5 年的任务可以识别 87% 的大于 1 亿吨的潜在撞击(托里诺-9,"区域破坏")。如果执行 10 年的任务,这一比例将提高到 94%。我们还展示了预警时间的分布如何随撞击能量而变化。
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引用次数: 0
Thermodynamic Predictions of Hydrogen Generation during the Serpentinization of Harzburgite with Seawater-derived Brines 海水卤水蛇床子化过程中氢气生成的热力学预测
Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-06-19 DOI: 10.3847/psj/ad42a1
Sanjoy M. Som, Serhat Sevgen, Adam A. Suttle, Jeff S. Bowman and Britney E. Schmidt
Salty aqueous solutions (brines) occur on Earth and may be prevalent elsewhere. Serpentinization represents a family of geochemical reactions where the hydration of olivine-rich rocks can release aqueous hydrogen, H2(aq), as a byproduct, and hydrogen is a known basal electron donor for terrestrial biology. While the effects of lithological differences on serpentinization products have been thoroughly investigated, effects focusing on compositional differences of the reacting fluid have received less attention. In this contribution, we investigate how the chemistry of seawater-derived brines affects the generation of biologically available hydrogen resulting from the serpentinization of harzburgite. We numerically investigate the serpentinization of ultramafic rocks at equilibrium with an array of brines at different water activities (a proxy for salt concentration in aqueous fluids and a determinant for habitability) derived from seawater evaporation. Because the existing supersaturation of aqueous calcium carbonate, a contributor to dissolved inorganic carbon (DIC) in natural seawater, cannot be captured in equilibrium calculations, we bookend our calculations by enabling and suppressing carbonate minerals when simulating serpentinization. We find that the extent of DIC supersaturation can provide an important control of hydrogen availability. Increased DIC becomes a major sink for hydrogen by producing formate and associated complexes when the reacting fluids are acidic enough to allow for CO2. Indeed, H2(aq) reduces CO2(aq) to formate, leading to a hydrogen deficit. These conclusions provide additional insights into the habitability of brine systems, given their potential for serpentinization across diverse planetary bodies such as on Mars and ocean worlds.
地球上存在含盐水溶液(盐水),其他地方也可能普遍存在。蛇纹石化是地球化学反应的一种,富含橄榄石的岩石在水化过程中会释放出水溶液氢(H2(aq))作为副产品,而氢是已知的陆地生物的基本电子供体。虽然岩性差异对蛇纹石化产物的影响已得到深入研究,但反应流体成分差异的影响却较少受到关注。在这篇论文中,我们研究了海水衍生盐水的化学性质如何影响哈兹堡垒岩蛇纹石化过程中产生的生物可用氢。我们用数值方法研究了超基性岩在与一系列不同水活度的盐水(水流中盐浓度的代表和可居住性的决定因素)达到平衡时的蛇纹石化过程。碳酸钙是天然海水中溶解无机碳(DIC)的成因之一,由于平衡计算无法捕捉到碳酸钙水溶液的过饱和度,因此我们在模拟蛇化过程中通过启用和抑制碳酸盐矿物来对计算进行补充。我们发现,DIC 过饱和的程度可以对氢的可用性起到重要的控制作用。当反应流体的酸性足以允许二氧化碳进入时,DIC的增加会产生甲酸盐和相关的络合物,从而成为氢的主要吸收汇。事实上,H2(aq)会将 CO2(aq)还原成甲酸盐,从而导致氢气不足。考虑到盐水系统在火星和海洋世界等不同行星体中的蛇床子化潜力,这些结论为盐水系统的宜居性提供了更多启示。
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引用次数: 0
Retrieved Atmospheres and Inferred Surface Properties for Terrestrial Exoplanets Using Transmission and Reflected-light Spectroscopy 利用透射和反射光分光镜检索类地系外行星的大气层和推断表面性质
Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-06-18 DOI: 10.3847/psj/ad381e
Samantha Gilbert-Janizek, Victoria S. Meadows and Jacob Lustig-Yaeger
Future astrophysics missions will seek extraterrestrial life via transmission and direct-imaging observations. To assess habitability and biosignatures, we need robust retrieval tools to analyze observed spectra, and infer surface and atmospheric properties with their uncertainties. We use a novel retrieval tool to assess accuracy in characterizing near-surface habitability and biosignatures via simulated transmission and direct-imaging spectra, based on the Origins Space Telescope (Origins) and LUVOIR mission concepts. We assess our ability to discriminate between an Earth-like and a false-positive O3 TRAPPIST-1 e with transmission spectroscopy. In reflected light, we assess the robustness of retrieval results to unmodeled cloud extinction. We find that assessing habitability using transmission spectra may be challenging due to relative insensitivity to surface temperature and near-surface H2O abundances. Nonetheless, our order-of-magnitude H2O constraints can discriminate extremely desiccated worlds. Direct imaging is insensitive to surface temperature and subject to the radius/albedo degeneracy, but this method proves highly sensitive to surface water abundance, achieving retrieval precision within 0.1% even with partial clouds. Concerning biosignatures, Origins-like transmission observations (t = 40 hr) may detect the CO2/CH4 pair on M-dwarf planets and differentiate between biological and false-positive O3 using H2O and abundant CO. In contrast, direct-imaging observations with LUVOIR-A (t = 10 hr) are better suited to constraining O2 and O3, and may be sensitive to wavelength-dependent water cloud features, but will struggle to detect modern-Earth-like abundances of methane. For direct imaging, we weakly detect a stratospheric ozone bulge by fitting the near-UV wings of the Hartley band.
未来的天体物理学任务将通过传输和直接成像观测来寻找地外生命。为了评估宜居性和生物特征,我们需要强大的检索工具来分析观测到的光谱,并推断表面和大气属性及其不确定性。我们根据起源太空望远镜(Origins)和 LUVOIR 任务概念,使用一种新颖的检索工具来评估通过模拟透射和直接成像光谱来描述近表面宜居性和生物特征的准确性。我们评估了利用透射光谱辨别类地和假阳性 O3 TRAPPIST-1 e 的能力。在反射光下,我们评估了检索结果对未建模云消光的稳健性。我们发现,由于对表面温度和近表面 H2O 丰度相对不敏感,利用透射光谱评估宜居性可能具有挑战性。尽管如此,我们的数量级 H2O 约束条件还是可以分辨出极度干燥的世界。直接成像法对表面温度不敏感,而且受半径/反照率退化的影响,但这种方法被证明对表面水丰度高度敏感,即使在有部分云层的情况下,检索精度也能达到0.1%以内。关于生物特征,类似起源的透射观测(t = 40 小时)可以探测到 M-矮行星上的 CO2/CH4 对,并利用 H2O 和丰富的 CO 区分生物 O3 和假阳性 O3。相比之下,利用 LUVOIR-A 进行的直接成像观测(t = 10 小时)更适于对 O2 和 O3 进行约束,并可能对波长相关的水云特征很敏感,但很难探测到类似现代地球的甲烷丰度。在直接成像方面,我们通过拟合哈特利波段的近紫外翼,微弱地探测到了平流层臭氧隆起。
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引用次数: 0
Energy and Temperature Dependencies for Electron-induced Sputtering from H2O Ice: Implications for the Icy Galilean Moons 来自 H2O 冰的电子诱导溅射的能量和温度依赖性:对冰冷的伽利略卫星的影响
Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-06-17 DOI: 10.3847/psj/ad484d
Rebecca A. Carmack and Mark J. Loeffler
To better assess the role that electrons play in exosphere production on icy bodies, we measured the total and O2 sputtering yields from H2O ice for electrons with energies between 0.75 and 10 keV and temperatures between 15 and 124.5 K. We find that both total and O2 yields increase with decreasing energy over our studied range, that they increase rapidly at temperatures above 60 K, and that the relative amount of H2O in the sputtered flux decreases quickly with increasing energy. Combining our data with other electron data in the literature, we show that the accuracy of a widely used sputtering model can be improved significantly for electrons by adjusting some of the intrinsic parameter values. Applying our results to Europa, we estimate that the contribution of electrons to the production of the O2 exosphere is equal to the combined contribution of all ions. In contrast, sputtering of O2 from Ganymede and Callisto appears to be dominated by irradiating ions, though electrons still likely contribute a nonnegligible amount. While our estimates could be further refined by examining the importance of spatial variations in electron flux, we conclude that, at the very least, electrons seem to be important for exosphere production on icy surfaces and should be included in future modeling efforts.
为了更好地评估电子在冰体外大气层产生过程中的作用,我们测量了能量在0.75到10 keV之间、温度在15到124.5 K之间的电子从H2O冰中溅射出的总产率和O2产率。我们发现,在我们研究的范围内,总产率和O2产率都随着能量的降低而增加,在温度高于60 K时,它们迅速增加,而且溅射通量中的H2O相对量随着能量的增加而迅速减少。结合我们的数据和文献中的其他电子数据,我们表明,通过调整一些固有参数值,可以显著提高广泛使用的电子溅射模型的准确性。将我们的结果应用于欧罗巴星,我们估计电子对产生 O2 外大气层的贡献等于所有离子贡献的总和。相比之下,来自木卫二和卡利斯托的O2溅射似乎主要是由辐照离子产生的,尽管电子的贡献可能仍然不可忽略。虽然可以通过研究电子通量空间变化的重要性来进一步完善我们的估算,但我们得出的结论是,至少电子似乎对冰表面外大气层的产生很重要,应将其纳入未来的建模工作中。
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引用次数: 0
Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration 月球南极附近阿蒙森环形山区域的地质历史:未来探索的基础
Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-06-17 DOI: 10.3847/psj/ad2c04
Lukas Wueller, Wajiha Iqbal, Thomas Frueh, Carolyn H. van der Bogert and Harald Hiesinger
We provide the first detailed 1:100,000 scale geomorphologic map of the ∼100 km Amundsen crater region, which is of high scientific relevance for future exploration, e.g., NASA’s VIPER mission, the Artemis program, and the Chinese International Lunar Research Station. We investigated the complex geological history of the region before and after the formation of Amundsen crater on the rims of the South Pole–Aitken (SPA) and Amundsen–Ganswindt basins. We present a new Amundsen crater formation age of ∼4.04 Ga, which, in contrast to previously derived ages, is based on non-light-plains terrain. The estimated maximum excavation depth for Amundsen crater is ∼8 km, and elevated concentrations of FeO near the crater suggest that Amundsen may have redistributed SPA-derived materials. Plains materials of various kinds were observed both inside and outside Amundsen crater and are estimated to be up to 350 m thick and ∼3.8 Ga old. A less cratered, tens of meters thick mantling unit indicates a resurfacing event ∼3.7 Ga ago. We highlight five potential exploration sites that satisfy technical constraints (such as shallow slopes, solar illumination, and Earth visibility), provide materials that can be sampled, and are capable of addressing multiple science objectives. Due to its accessibility and traversability, combined with its geologic diversity, proximity of permanently shadowed regions for studying volatile processes, and ability to address multiple science objectives, we confirm and reinforce the Amundsen crater region as a high-priority landing and exploration site.
我们提供了第一张1:100,000比例尺的阿蒙森陨石坑区域详细地貌图,该区域对未来的探索(如美国国家航空航天局的VIPER任务、阿特米斯计划和中国国际月球研究站)具有重要的科学意义。我们研究了南极-艾特肯盆地(SPA)和阿蒙森-甘斯文特盆地边缘阿蒙森环形山形成前后该地区复杂的地质历史。我们提出了一个新的阿蒙森陨石坑形成年龄,即4.04Ga∼4.04Ga,与之前推算的年龄不同,这个年龄是基于非光原地形推算出来的。据估计,阿蒙森陨石坑的最大挖掘深度为8千米,陨石坑附近高浓度的氧化铁表明,阿蒙森陨石坑可能重新分布了SPA衍生物质。在阿蒙森陨石坑内外都观察到了不同种类的平原物质,据估计厚度可达350米,年龄在3.8千兆年前。一个火山口较少、几十米厚的地幔单元表明,在距今3.7亿年前曾发生过一次地幔重现事件。我们重点介绍了五个潜在的勘探地点,这些地点满足技术上的限制(如浅斜坡、太阳光照和地球能见度),提供可采样的材料,并能实现多个科学目标。由于阿蒙森陨石坑地区交通便利、易于穿越,再加上其地质多样性、临近用于研究挥发过程的永久阴影区以及能够实现多种科学目标,我们确认并加强了该地区作为一个高度优先的着陆和勘探地点的地位。
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引用次数: 0
Constraining Time Variations in Enceladus’s Water-vapor Plume with Near-infrared Spectra from Cassini’s Visual and Infrared Mapping Spectrometer 利用卡西尼号可见光和红外绘图分光计的近红外光谱确定土卫二水汽羽流的时间变化
Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-06-16 DOI: 10.3847/psj/ad4c69
K. E. Denny, M. M. Hedman, D. Bockelée-Morvan, G. Filacchione and F. Capaccioni
Water vapor produces a series of diagnostic emission lines in the near-infrared between 2.60 and 2.75 μm. The Visual and Infrared Mapping Spectrometer (VIMS) on board the Cassini spacecraft detected this emission signal from Enceladus’s plume, and so VIMS observations provide information about the variability of the plume’s water-vapor content. Using a data set of 249 spectral cubes with relatively high signal-to-noise ratios, we confirmed the strength of this water-vapor emission feature corresponds to a line-of-sight column density of order 1020 molecules m−2, which is consistent with previous measurements from Cassini’s Ultraviolet Imaging Spectrograph. Comparing observations made at different times indicates that the water-vapor flux is unlikely to vary systematically with Enceladus’s orbital phase, unlike the particle flux, which does vary with orbital phase. However, variations in the column density on longer and shorter timescales cannot be ruled out and merit further investigation.
水蒸气在 2.60 和 2.75 μm 之间的近红外波段产生一系列诊断发射线。卡西尼号飞船上的可见光和红外绘图分光仪(VIMS)探测到了来自恩克拉多斯羽流的这一发射信号,因此可见光和红外绘图分光仪的观测提供了有关羽流水蒸气含量变化的信息。我们利用信噪比相对较高的 249 个光谱立方体数据集,确认了这一水蒸气发射特征的强度与 1020 分子 m-2 量级的视线柱密度相对应,这与卡西尼号紫外线成像分光仪之前的测量结果一致。比较不同时间的观测结果表明,水蒸气通量不太可能随着恩克拉多斯轨道相位的变化而系统地变化,这与粒子通量不同,后者确实会随着轨道相位的变化而变化。不过,不能排除水柱密度在较长和较短时间尺度上的变化,这值得进一步研究。
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引用次数: 0
The Limited Role of the Streaming Instability during Moon and Exomoon Formation 流不稳定性在月球和外月形成过程中的有限作用
Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-06-16 DOI: 10.3847/psj/ad4863
Miki Nakajima, Jeremy Atkins, Jacob B. Simon and Alice C. Quillen
It is generally accepted that the Moon accreted from the disk formed by an impact between the proto-Earth and impactor, but its details are highly debated. Some models suggest that a Mars-sized impactor formed a silicate melt-rich (vapor-poor) disk around Earth, whereas other models suggest that a highly energetic impact produced a silicate vapor-rich disk. Such a vapor-rich disk, however, may not be suitable for the Moon formation, because moonlets, building blocks of the Moon, of 100 m–100 km in radius may experience strong gas drag and fall onto Earth on a short timescale, failing to grow further. This problem may be avoided if large moonlets (≫100 km) form very quickly by streaming instability, which is a process to concentrate particles enough to cause gravitational collapse and rapid formation of planetesimals or moonlets. Here, we investigate the effect of the streaming instability in the Moon-forming disk for the first time and find that this instability can quickly form ∼100 km-sized moonlets. However, these moonlets are not large enough to avoid strong drag, and they still fall onto Earth quickly. This suggests that the vapor-rich disks may not form the large Moon, and therefore the models that produce vapor-poor disks are supported. This result is applicable to general impact-induced moon-forming disks, supporting the previous suggestion that small planets (<1.6 R⊕) are good candidates to host large moons because their impact-induced disks would likely be vapor-poor. We find a limited role of streaming instability in satellite formation in an impact-induced disk, whereas it plays a key role during planet formation.
人们普遍认为,月球是由原地球和撞击器之间的撞击所形成的圆盘吸积而成的,但其细节却存在很大争议。一些模型认为,火星大小的撞击器在地球周围形成了一个富含硅酸盐熔体(蒸汽贫乏)的圆盘,而另一些模型则认为,高能撞击产生了一个富含硅酸盐蒸汽的圆盘。然而,这种富含水汽的圆盘可能并不适合月球的形成,因为半径为 100 米至 100 千米的小卫星(月球的组成部分)可能会受到强大的气体阻力,在短时间内坠落到地球上,无法继续生长。如果大型小月体(≫100 千米)通过流不稳定性迅速形成,这个问题就可以避免。流不稳定性是一个将粒子集中到足以导致引力塌缩并迅速形成小行星或小月的过程。在这里,我们首次研究了成月盘中流不稳定性的影响,发现这种不稳定性可以快速形成∼100 公里大小的小月。然而,这些小月并没有大到足以避开强大阻力的程度,它们仍然会很快落到地球上。这表明富含蒸汽的磁盘可能不会形成大卫星,因此产生贫蒸汽磁盘的模型得到了支持。这一结果适用于一般的撞击诱发的卫星形成盘,支持了之前的建议,即小行星(<1.6 R⊕)是承载大卫星的良好候选者,因为它们的撞击诱发盘很可能是贫蒸汽的。我们发现流不稳定性在撞击诱发盘中卫星形成过程中的作用有限,而在行星形成过程中却起着关键作用。
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引用次数: 0
Discovery and Classification in Astronomy: Scientific and Philosophical Challenges and the Importance of a Comprehensive and Consistent Classification System 天文学的发现与分类:天文学的发现与分类:科学与哲学的挑战以及全面一致的分类系统的重要性
Q2 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-06-12 DOI: 10.3847/psj/ad4edd
Steven J. Dick
Throughout history, the definition of “class” and the construction of astronomical classification systems has been a deep scientific and philosophical problem: scientific because facts such as physical composition ideally need to be known for proper classification but often are not, philosophical because astronomers need to understand the philosophical assumptions behind their attempts at classification, and because different philosophical ideas such as “natural kinds” often guide classification, even if unconsciously. The primary lesson of history is that the most useful classifications of celestial objects are optimally based on their physical nature. The second lesson is that because discovery is an extended process consisting of detection, interpretation, and understanding, initial classifications may be phenomenological, based on characteristics that may be useful in early “detection” stages of extended discovery. By contrast, final classifications of “the thing itself,” is achieved only after the “understanding” stage of discovery and must have a physical basis. A third lesson is that class status is best determined within a comprehensive classification system in order to determine taxon level, e.g., class, type, subtype. Such a system, encompassing all astronomical objects, illustrates the problems of class and classification, problems that may be applied to exoplanet discoveries.
纵观历史,"类 "的定义和天文分类系统的构建一直是一个深奥的科学和哲学问题:科学性是因为理想情况下需要知道物理成分等事实才能进行正确的分类,但事实往往并非如此;哲学性是因为天文学家需要理解其分类尝试背后的哲学假设,还因为 "自然种类 "等不同的哲学观点往往指导着分类,即使是无意识的。历史的主要教训是,最有用的天体分类最好是基于天体的物理本质。第二个教训是,由于发现是一个由探测、解释和理解组成的扩展过程,最初的分类可能是现象学的,基于在扩展发现的早期 "探测 "阶段可能有用的特征。相比之下,"事物本身 "的最终分类只有在发现的 "理解 "阶段之后才能实现,而且必须有物理基础。第三个经验是,最好在一个全面的分类系统中确定类别地位,以确定分类群的级别,如类、型、亚型。这样一个涵盖所有天文物体的系统说明了类和分类的问题,这些问题可能适用于系外行星的发现。
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引用次数: 0
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