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A continuum from clear to cloudy hot-Jupiter exoplanets without primordial water depletion

机译：从清澈到浑浊的热木星系外行星的连续过程，而没有原始水的消耗

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摘要

Thousands of transiting exoplanets have been discovered, but spectral analysis of their atmospheres has so far been dominated by a small number of exoplanets and data spanning relatively narrow wavelength ranges (such as 1.1-1.7 micrometres). Recent studies show that some hot-Jupiter exoplanets have much weaker water absorption features in their near-infrared spectra than predicted(1-5). The low amplitude of water signatures could be explained by very low water abundances(6-8), which may be a sign that water was depleted in the protoplanetary disk at the planet's formation location9, but it is unclear whether this level of depletion can actually occur. Alternatively, these weak signals could be the result of obscuration by clouds or hazes(1-4), as found in some optical spectra(3,4,10,11). Here we report results from a comparative study of ten hot Jupiters covering the wavelength range 0.3-5 micrometres, which allows us to resolve both the optical scattering and infrared molecular absorption spectroscopically. Our results reveal a diverse group of hot Jupiters that exhibit a continuum from clear to cloudy atmospheres. We find that the difference between the planetary radius measured at optical and infrared wavelengths is an effective metric for distinguishing different atmosphere types. The difference correlates with the spectral strength of water, so that strong water absorption lines are seen in clear-atmosphere planets and the weakest features are associated with clouds and hazes. This result strongly suggests that primordial water depletion during formation is unlikely and that clouds and hazes are the cause of weaker spectral signatures.
机译：已经发现了成千上万个正在飞行的系外行星，但是到目前为止，对它们大气的光谱分析一直被少数系外行星和跨越相对窄的波长范围（例如1.1-1.7微米）的数据所控制。最近的研究表明，一些热的木星系外行星在其近红外光谱中的吸水特征比预测的要弱得多（1-5）。水分信号的低振幅可以用非常低的水丰度来解释（6-8），这可能表明水在行星形成位置的原行星盘中已经耗尽9，但目前尚不清楚这种耗尽水平是否可以发生。或者，这些弱信号可能是由于云或雾霾（1-4）所遮挡的结果，如某些光谱（3,4,10,11）所示。在这里，我们报告了对十个热木星的比较研究的结果，这些木星的波长范围为0.3-5微米，这使我们能够从光谱上解析光学散射和红外分子吸收。我们的结果揭示了一组不同的热木星，这些木星表现出从晴朗到阴天的连续性。我们发现，在光学和红外波长下测得的行星半径之间的差异是区分不同大气类型的有效指标。差异与水的光谱强度有关，因此在大气层清晰的行星上可以看到强的吸水线，而最薄弱的特征与云层和阴霾有关。这一结果有力地表明，在形成过程中原始水的消耗是不可能的，并且云雾和阴霾是光谱特征减弱的原因。

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  • 来源
    《Nature》 |2016年第7584期|59-62|共4页
  • 作者

    Sing David K.; Fortney Jonathan J.; Nikolov Nikolay; Wakeford Hannah R.; Kataria Tiffany; Evans Thomas M.; Aigrain Suzanne; Ballester Gilda E.; Burrows Adam S.; Deming Drake; Desert Jean-Michel; Gibson Neale P.; Henry Gregory W.; Huitson Catherine M.; Knutson Heather A.; des Etangs Alain Lecavelier; Pont Frederic; Showman Adam P.; Vidal-Madjar Alfred; Williamson Michael H.; Wilson Paul A.;

  • 作者单位

    Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England;

    Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA;

    Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England;

    Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England;

    Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England;

    Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England;

    Univ Oxford, Dept Phys, Keble Rd, Oxford OX1 3RH, England;

    Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA;

    Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA;

    Univ Maryland, Dept Astron, College Pk, MD 20742 USA;

    Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA;

    European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany;

    Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA;

    Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA;

    CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA;

    CNRS, Inst Astrophys Paris, UMR 7095, 98 Bis Blvd Arago, F-75014 Paris, France;

    Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England;

    Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA;

    CNRS, Inst Astrophys Paris, UMR 7095, 98 Bis Blvd Arago, F-75014 Paris, France;

    Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA;

    CNRS, Inst Astrophys Paris, UMR 7095, 98 Bis Blvd Arago, F-75014 Paris, France;

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