论文标题
热jupiter气氛中的各种朦胧条件
A large range of haziness conditions in hot-Jupiter atmospheres
论文作者
论文摘要
我们介绍了基于自洽模型，包括雾化微物理学，不平衡化学和辐射反馈的基础模型的系外行星大气的光化学危险的研究。我们得出了匹配十个热jupiter的HST观测所需的雾化特性。 HAT-P-12B，HD-189733B，HD-209458B和WASP-6B需要5x10 $^{ - 15} $和9x10 $^{ - 12} g.cm^{ - 2} g.cm^{ - 2} .s^{ - 1} $之间的雾质质量通量。 WASP-12b和WASP-19b具有平衡温度高于2000 K的温度与雾兹的存在不相容，并且重金属更好地适合。 HAT-P-1B和WASP-31B没有明确证据表明存在具有10 $^{ - 15} $和10 $^{ - 16} g.cm^{ - 2} .s^{ - 1} $的HAZE的危险，而wasp-17b和Wasp-39b的上质量是10 $ 16} - 16} - 16} - { - 1} $。 g.cm^{ - 2} .s^{ - 1} $。我们讨论了自洽模型的含义，并根据光化学结果得出了雾化丰度的上限。我们的结果表明，HCN是最高1300 K有效温度的主要雾度前体和上面的CO。我们基于对观测的拟合度的衍生雾质质量通量与光化学一致，形成的产量高达$ \ sim $ 6.4 \％。考虑到使用的低分辨率观察结果，不平衡化学对光谱的影响忽略不计，但会影响化学成分和温度曲线。我们发现，Hazes会产生更热的上层大气温度，并对光谱产生可检测的影响。云可能对解释HD-209458B，WASP-31B和WASP-39B的过境光谱有影响。然而，除WASP-12B和WASP-19B以外，所有研究的气氛中都有硅酸盐和铁云的存在。
We present a study of photochemical hazes of exoplanet atmospheres based on a self-consistent model including haze microphysics, disequilibrium chemistry, and radiative feedbacks. We derive the haze properties required to match HST observations of ten hot-Jupiters. HAT-P-12b, HD-189733b, HD-209458b and WASP-6b require haze mass fluxes between 5x10$^{-15}$ and 9x10$^{-12} g.cm^{-2}.s^{-1}$ to match the observations. WASP-12b and WASP-19b with equilibrium temperatures above 2000 K are incompatible with the presence of haze and are better fitted by heavy metals. HAT-P-1b and WASP-31b do not show clear evidence for the presence of hazes with upper mass fluxes of 10$^{-15}$ and 10$^{-16}g.cm^{-2}.s^{-1}$, respectively, while WASP-17b and WASP-39b present an upper mass flux limit of 10$^{-16} g.cm^{-2}.s^{-1}$. We discuss the implications of the self-consistent model and we derive upper limits for the haze abundances based on photochemistry results. Our results suggest HCN as the main haze precursor up to 1300 K effective temperatures and CO above. Our derived haze mass fluxes based on the fit to the observations are consistent with the photochemistry with formation yields up to $\sim$6.4\%. Disequilibrium chemistry has negligible impact on the spectra considering the low resolution observations used but impacts the chemical composition and temperature profiles. We find that hazes produce hotter upper atmosphere temperatures with a detectable impact on the spectra. Clouds may have implications for interpreting the transit spectra of HD-209458b, WASP-31b and WASP-39b. Nevertheless, the presence of silicate and iron clouds is expected in all studied atmospheres except WASP-12b and WASP-19b.
