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Measuring the D/H Ratios of Exoplanets and Brown Dwarfs

  • Authors: Caroline V. Morley, Andrew J. Skemer, Brittany E. Miles, Michael R. Line, Eric D. Lopez, Matteo Brogi, Richard S. Freedman, and Mark S. Marley

2019 The Astrophysical Journal Letters 882 L29.

  • Provider: AAS Journals

Caption: Figure 5.

Top panel: model spectra, offset for clarity, of a 320 K, g = 15 m s−2, cloud-free object; top model is solar metallicity, with no CH3D (gray line) and a protosolar (2 × 10−5) D/H ratio (purple line); bottom model is 100× solar metallicity with no CH3D (gray line) and enhanced (5 × 10−5) D/H ratio (pink line). Middle panel: S/N per spectral element needed to detect CH3D as a function of metallicity for protosolar and enhanced D/H ratios for a planet with T = 320 K, g = 15 m s−2. CH3D is easier to detect in high-metallicity objects and for enhanced D/H ratios. Regions are shaded according to the metallicities of local brown dwarfs and solar system giant planets. Bottom panel: intrinsic temperatures of model planets over time for solar and 50× solar metallicity atmospheric boundary conditions, assuming a 20% H/He planet by mass. The 320 K temperature modeled above corresponds to a 20 Myr Saturn-mass planet or a 1–2 Myr super-Neptune.

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