木星大红斑上层着色剂雾霾的微物理模型
Microphysical Model of Jupiter's Great Red Spot Upper Chromophore Haze
AI总结：
本研究通过微物理模拟揭示木星大红斑上层雾霾的形成机制，发现其需要特定的注入通量和时间尺度，且消光由单一对数正态分布的粒子主导。
摘要：
木星大红斑（GRS）的红色着色起源是行星科学中的长期问题。尽管已经提出几种候选着色剂，但对其本质、演变和与大气动力学关系仍无明确结论。在本工作中，我们对GRS上层的红色雾霾进行了微物理模拟，并量化了维持其所需的生产率和时间尺度。为了匹配之前报告的着色剂柱质量及有效半径，需要柱积分注入通量在$1\times10^{-12}$-$7\times10^{-12}$ kg m$^{-2}$ s$^{-1}$范围内，这要求上层对流层中低上升速度（$v_{\mathrm{trop}}\lesssim 1.5\times10^{-4}$ m s$^{-1}$）和每微米至少20个电子的电荷。此类速率超过了标准的木星photochemical模型通过NH$_3$-C$_2$H$_2$光化学反应在0.1-0.2 bar处提供的质量通量，这是近期文献中最流行的着色剂路径。我们发现雾霾形成时间的下限为7年。我们还评估了常用大小和垂直分布参数化方法，发现涡旋扩散阻止了薄层的长期限制，并且消光主要由可由单一对数正态大小分布表示的粒子主导。
英文摘要：
The origin of the red colouration in Jupiter's Great Red Spot (GRS) is a long-standing question in planetary science. While several candidate chromophores have been proposed, no clear conclusions have been reached regarding its nature, evolution, or relationship to atmospheric dynamics. In this work, we perform microphysical simulations of the reddish haze over the GRS and quantify the production rates and timescales required to sustain it. Matching the previously reported chromophore column mass and effective radius in the GRS requires column-integrated injection fluxes in the range $1\times10^{-12}$-$7\times10^{-12}$ kg m$^{-2}$ s$^{-1}$, under low upwelling velocities in the upper troposphere ($v_{\mathrm{trop}}\lesssim 1.5\times10^{-4}$ m s$^{-1}$) and particle charges of at least 20 electrons per $μ$m. Such rates exceed the mass flux that standard photochemical models of Jupiter currently supply via NH$_3$-C$_2$H$_2$ photochemistry at 0.1-0.2 bar, the most popular chromophore pathway in recent literature. We find a lower limit of 7 years on the haze formation time. We also assess commonly used size and vertical distribution parameterisations for the chromophore haze, finding that eddy diffusion prevents the long-term confinement of a thin layer and that the extinction is dominated by particles that can be represented by a single log-normal size distribution.
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