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朦胧的蓝色世界：天王星和海王星的整体气溶胶模型，包括暗斑。

Hazy Blue Worlds: A Holistic Aerosol Model for Uranus and Neptune, Including Dark Spots.

作者信息

Irwin P G J, Teanby N A, Fletcher L N, Toledo D, Orton G S, Wong M H, Roman M T, Pérez-Hoyos S, James A, Dobinson J

机构信息

Department of Physics University of Oxford Oxford UK.

School of Earth Sciences University of Bristol Bristol UK.

出版信息

J Geophys Res Planets. 2022 Jun;127(6):e2022JE007189. doi: 10.1029/2022JE007189. Epub 2022 Jun 4.

DOI:10.1029/2022JE007189
PMID:35865671
原文链接:https://pmc.ncbi.nlm.nih.gov/articles/PMC9286428/
Abstract

We present a reanalysis (using the Minnaert limb-darkening approximation) of visible/near-infrared (0.3-2.5 μm) observations of Uranus and Neptune made by several instruments. We find a common model of the vertical aerosol distribution i.e., consistent with the observed reflectivity spectra of both planets, consisting of: (a) a deep aerosol layer with a base pressure >5-7 bar, assumed to be composed of a mixture of HS ice and photochemical haze; (b) a layer of photochemical haze/ice, coincident with a layer of high static stability at the methane condensation level at 1-2 bar; and (c) an extended layer of photochemical haze, likely mostly of the same composition as the 1-2-bar layer, extending from this level up through to the stratosphere, where the photochemical haze particles are thought to be produced. For Neptune, we find that we also need to add a thin layer of micron-sized methane ice particles at ∼0.2 bar to explain the enhanced reflection at longer methane-absorbing wavelengths. We suggest that methane condensing onto the haze particles at the base of the 1-2-bar aerosol layer forms ice/haze particles that grow very quickly to large size and immediately "snow out" (as predicted by Carlson et al. (1988), https://doi.org/10.1175/1520-0469(1988)045<2066:CMOTGP>2.0.CO;2), re-evaporating at deeper levels to release their core haze particles to act as condensation nuclei for HS ice formation. In addition, we find that the spectral characteristics of "dark spots", such as the Voyager-2/ISS Great Dark Spot and the HST/WFC3 NDS-2018, are well modelled by a darkening or possibly clearing of the deep aerosol layer only.

摘要

我们对几台仪器对天王星和海王星进行的可见光/近红外（0.3 - 2.5微米）观测进行了重新分析（使用米纳尔特临边昏暗近似法）。我们发现了一个垂直气溶胶分布的通用模型，即与两颗行星观测到的反射光谱一致，该模型由以下部分组成：(a) 一个深层气溶胶层，底部压力>5 - 7巴，假定由硫化氢冰和光化学霾的混合物组成；(b) 一层光化学霾/冰，与1 - 2巴甲烷凝结层处的高静力稳定层重合；(c) 一层延伸的光化学霾层，其成分可能与1 - 2巴层基本相同，从该层向上延伸至平流层，光化学霾颗粒被认为是在平流层产生的。对于海王星，我们发现还需要在约0.2巴处添加一层微米级的甲烷冰颗粒，以解释在较长甲烷吸收波长处增强的反射。我们认为，在1 - 2巴气溶胶层底部凝结在霾颗粒上的甲烷形成了冰/霾颗粒，这些颗粒迅速长大到很大尺寸并立即“沉降”（如卡尔森等人（1988年）所预测，https://doi.org/10.1175/1520 - 0469(1988)045<2066:CMOTGP>2.0.CO;2），在更深层重新蒸发，释放出其核心霾颗粒，作为形成硫化氢冰的凝结核。此外，我们发现，“暗斑”的光谱特征，如“旅行者2号”/成像科学子系统大黑斑和哈勃太空望远镜/第三代广域相机3的NDS - 2018，仅通过深层气溶胶层的变暗或可能的变清就能很好地模拟。

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本文引用的文献

1
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2
Microwave observations reveal the deep extent and structure of Jupiter's atmospheric vortices.微波观测揭示了木星大气涡旋的深远范围和结构。
Science. 2021 Nov 19;374(6570):968-972. doi: 10.1126/science.abf1015. Epub 2021 Oct 28.
3
Atmospheric chemistry on Uranus and Neptune.天王星和海王星上的大气化学。
Nat Commun. 2023 Feb 27;14(1):1104. doi: 10.1038/s41467-023-36841-1.
4
Seeking answers, planetary scientists plot a return to the nearest ice giant.
Proc Natl Acad Sci U S A. 2022 Nov;119(44):e2216692119. doi: 10.1073/pnas.2216692119. Epub 2022 Oct 20.
Philos Trans A Math Phys Eng Sci. 2020 Dec 25;378(2187):20190477. doi: 10.1098/rsta.2019.0477. Epub 2020 Nov 9.
4
Neptune and Uranus: ice or rock giants?海王星和天王星：冰巨星还是岩质巨星？
Philos Trans A Math Phys Eng Sci. 2020 Dec 25;378(2187):20190489. doi: 10.1098/rsta.2019.0489. Epub 2020 Nov 9.
5
Remote determination of the shape of Jupiter's vortices from laboratory experiments.通过实验室实验远程确定木星漩涡的形状。
Nat Phys. 2020 Jun;16(6):695-700. doi: 10.1038/s41567-020-0833-9. Epub 2020 Mar 16.
6
Matrix operator theory of radiative transfer. 1: rayleigh scattering.辐射传输的矩阵算子理论。1：瑞利散射。
Appl Opt. 1973 Feb 1;12(2):314-29. doi: 10.1364/AO.12.000314.
7
Hubble Space Telescope Imaging of Neptune's Cloud Structure in 1994.哈勃空间望远镜于 1994 年对海王星云层结构的观测。
Science. 1995 Jun 23;268(5218):1740-2. doi: 10.1126/science.268.5218.1740.
8
Voyager 2 at neptune: imaging science results.“旅行者2号”在海王星：成像科学成果。
Science. 1989 Dec 15;246(4936):1422-49. doi: 10.1126/science.246.4936.1422.
9
The spectral sensitivities of the middle- and long-wavelength-sensitive cones derived from measurements in observers of known genotype.从中等波长敏感视锥细胞和长波长敏感视锥细胞的光谱敏感性是通过对已知基因型观察者的测量得出的。
Vision Res. 2000;40(13):1711-37. doi: 10.1016/s0042-6989(00)00021-3.
10
External supply of oxygen to the atmospheres of the giant planets.向气态巨行星大气层外部供应氧气。
Nature. 1997 Sep 11;389(6647):159-62. doi: 10.1038/38236.