论文标题
巨型行星木星大气中的水蒸气的阿尔玛光谱检测
ALMA spectroscopic detection of water vapour in the atmosphere of the giant gas planet Jupiter
论文作者
论文摘要
在Jovian的大气中，1994年7月在44 $^\ Circ $ s碰撞后，首次检测到痕量物种。这些痕量物种中的大多数都是通过光谱毫米/毫米观测到的。在木星的大气中，痕量气体在具有异质和均匀化学反应，与辐射的相互作用和相变的大气化学中起重要作用。在这里，我们在木星大气中以频率$ν$ = 183.310 ghz的速度介绍了水的旋转排放线（h $ _ {2} $ o）的第一光谱检测，并使用分子过渡j = 3 $ _ {1,3} $ _ {1,3} $ _- $ 2 $ _ {2 $ _ {2,2,2,2} $使用ATACAMA大型米尔列（Alman）/sumpillimeter（alman/sumpilter）。水排放线的统计柱密度为n（h $ _ {2} $ O）$ \ sim $ 4 $ \ times $ 10 $^{15} $ cm $^{ - 2} $。 h $ _ {2} $ o的旋转发射线在木星的平流层中找到，$ \ geq $ 3 $σ$统计显着性。 h $ _ {2} $ o的列密度相对于h $ _ {2} $的分数丰度对应于f（h $ _ {2} $ o）$ \ sim $ 4 $ \ times $ 10 $ 10 $^{ - 9} $。
In the Jovian atmosphere, the trace species are detected for the first time after the collision of comet Shoemaker-Levy 9 near 44$^\circ$S in July 1994. Most of these trace species are detected with spectroscopic millimeter/submillimeter observation. In the atmosphere of Jupiter, trace gases play an important role in atmospheric chemistry with heterogeneous and homogeneous chemical reactions, interaction with radiation, and phase transition. Here we present the first spectroscopic detection of the rotational emission line of water (H$_{2}$O) in the atmosphere of Jupiter at frequency $ν$ = 183.310 GHz with molecular transition J = 3$_{1,3}$$-$2$_{2,2}$ using Atacama Large Millimeter/Submillimeter Array (ALMA). The statistical column density of water emission line is N(H$_{2}$O)$\sim$4$\times$10$^{15}$ cm$^{-2}$. The rotational emission line of H$_{2}$O is found in the stratosphere of Jupiter with $\geq$3$σ$ statistical significance. The column density of H$_{2}$O corresponds to the fractional abundance relative to H$_{2}$ is f(H$_{2}$O)$\sim$ 4$\times$10$^{-9}$.
