HD 209458 b的3.6-8.0 μ m宽带发射光谱：大气温度反转的证据
The 3.6-8.0 Micron Broadband Emission Spectrum of HD 209458b: Evidence for an Atmospheric Temperature Inversion
摘要：
我们使用斯皮策太空望远镜上的红外阵列相机（IRAC）估计了太阳系外行星HD 209458 b在3.6，4.5，5.8和8.0微米处的带通集成热辐射的强度。我们在所有四个带通中同时观测到一次二次日食，并发现相对日食深度分别为0.00094 +/- 0.00009、0.00213 +/- 0.00015、0.00301 +/- 0.00043和0.00240 +/- 0.00026。这些日食深度揭示了推断出的行星发射光谱的形状与标准大气模型的预测有很大的不同;相反，最合理的解释是在大气层中存在一个逆温层，导致在4.5和5.8微米的带通中有大量的水排放。这是第一次清楚地表明在热木星的大气层中存在这样的逆温层，因为以前对其他行星的观测似乎与没有这种逆温层的模型的预测相当吻合。
英文摘要：
We estimate the strength of the bandpass-integrated thermal emission from the extrasolar planet HD 209458b at 3.6, 4.5, 5.8, and 8.0 microns using the Infrared Array Camera (IRAC) on the Spitzer Space Telescope. We observe a single secondary eclipse simultaneously in all four bandpasses and find relative eclipse depths of 0.00094 +/- 0.00009, 0.00213 +/- 0.00015, 0.00301 +/- 0.00043, and 0.00240 +/- 0.00026, respectively. These eclipse depths reveal that the shape of the inferred emission spectrum for the planet differs significantly from the predictions of standard atmosphere models; instead the most plausible explanation would require the presence of an inversion layer high in the atmosphere leading to significant water emission in the 4.5 and 5.8 micron bandpasses. This is the first clear indication of such a temperature inversion in the atmosphere of a hot Jupiter, as previous observations of other planets appeared to be in reasonably good agreement with the predictions of models without such an inversion layer.
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