论文标题
h $ _2 $在超热木星气氛中的可行性
Detection Feasibility of H$_2$ in Ultra-hot Jupiter Atmospheres
论文作者
论文摘要
由于其极端特性，超热木星（UHJ）最近成为了几项大气研究的重点。尽管分子氢（h $ _2 $）在UHJ大气中起关键作用，但在系外行星上尚未直接检测到它。为了确定H $ _2 $检测通过Lyman和Werner乐队的传输光谱检测的可行性，我们以H $ _2 $旋转温度从2000 K到4000 K的旋转温度到4000 K到旋转A型A-Type星星的建模，每个范围从$ T_ {EFF} $ = 8,500 k} $ T_ $ = $ T_} $ = 10,100行星星温度组合在增加泊松噪声的同时，幅度从0.5％到2.0％不等。最后，我们将光谱与预期的大气H $ _2 $吸收模板相交。我们的结果表明，H $ _2 $检测当前设施，即哈勃太空望远镜。但是，h $ _2 $的直接大气传输光谱可以通过未来的紫外线旗舰任务可行。
Ultra-hot Jupiters (UHJs) have recently been the focus of several atmospheric studies due to their extreme properties. While molecular hydrogen (H$_2$) plays a key role in UHJ atmospheres, it has not been directly detected on an exoplanet. To determine the feasibility of H$_2$ detection via transmission spectroscopy of the Lyman and Werner bands, we modeled UHJ atmospheres with H$_2$ rotational temperatures varying from 2000 K to 4000 K orbiting A-type stars ranging from $T_{eff}$ = 8,500 K to $T_{eff}$ = 10,300 K. We present simulated transmission spectra for each planet-star temperature combination while adding Poisson noise varying in magnitude from 0.5% to 2.0%. Finally, we cross-correlated the spectra with expected atmospheric H$_2$ absorption templates for each temperature combination. Our results suggest that H$_2$ detection with current facilities, namely the Hubble Space Telescope, is not possible. However, direct atmospheric transmission spectroscopy of H$_2$ may be viable with future UV-capable flagship missions.
