期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 474, 期 4, 页码 5158-5185出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stx3015
关键词
techniques: spectroscopic; planets and satellites: atmospheres; planets and satellites: composition; planets and satellites: gaseous planets
资金
- Leverhulme Trust Research Project Grant
- University of Exeter College of Engineering, Mathematics and Physical Sciences PhD studentship
- European Research Council under the European Unions Seventh Framework Programme (FP7)/ERC grant [336792]
- University of Exeter
- NASA Astrobiology Program through the Nexus for Exoplanet System Science
- STFC
- Large Facilities Capital Fund of BIS
- STFC [1784036] Funding Source: UKRI
We present a grid of forward model transmission spectra, adopting an isothermal temperature-pressure profile, alongside corresponding equilibrium chemical abundances for 117 observationally significant hot exoplanets (equilibrium temperatures of 547-2710 K). This model grid has been developed using a 1D radiative-convective-chemical equilibrium model termed ATMO, with up-to-date high-temperature opacities. We present an interpretation of observations of 10 exoplanets, including best-fitting parameters and chi(2) maps. In agreement with previous works, we find a continuum from clear to hazy/cloudy atmospheres for this sample of hot Jupiters. The data for all the 10 planets are consistent with subsolar to solar C/O ratio, 0.005 to 10 times solar metallicity and water rather than methane-dominated infrared spectra. We then explore the range of simulated atmospheric spectra for different exoplanets, based on characteristics such as temperature, metallicity, C/O ratio, haziness and cloudiness. We find a transition value for the metallicity between 10 and 50 times solar, which leads to substantial changes in the transmission spectra. We also find a transition value of C/O ratio, from water to carbon species dominated infrared spectra, as found by previous works, revealing a temperature dependence of this transition point ranging from similar to 0.56 to similar to 1-1.3 for equilibrium temperatures from similar to 900 to similar to 2600 K. We highlight the potential of the spectral features of HCN and C2H2 to constrain the metallicities and C/O ratios of planets, using James Webb Space Telescope (JWST) observations. Finally, our entire grid (similar to 460 000 simulations) is publicly available and can be used directly with the JWST simulator PandExo for planning observations.
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