A solar C/O and sub-solar metallicity in a hot Jupiter atmosphere

Michael R. Line (), Matteo Brogi, Jacob L. Bean, Siddharth Gandhi, Joseph Zalesky, Vivien Parmentier, Peter Smith, Gregory N. Mace, Megan Mansfield, Eliza M.-R. Kempton, Jonathan J. Fortney, Evgenya Shkolnik, Jennifer Patience, Emily Rauscher, Jean-Michel Désert and Joost P. Wardenier
Additional contact information
Michael R. Line: Arizona State University
Matteo Brogi: University of Warwick
Jacob L. Bean: University of Chicago
Siddharth Gandhi: University of Warwick
Joseph Zalesky: Arizona State University
Vivien Parmentier: University of Oxford
Peter Smith: Arizona State University
Gregory N. Mace: University of Texas at Austin
Megan Mansfield: University of Chicago
Eliza M.-R. Kempton: University of Maryland
Jonathan J. Fortney: University of California
Evgenya Shkolnik: Arizona State University
Jennifer Patience: Arizona State University
Emily Rauscher: University of Michigan
Jean-Michel Désert: University of Amsterdam
Joost P. Wardenier: University of Oxford

Nature, 2021, vol. 598, issue 7882, 580-584

Abstract: Abstract Measurements of the atmospheric carbon (C) and oxygen (O) relative to hydrogen (H) in hot Jupiters (relative to their host stars) provide insight into their formation location and subsequent orbital migration1,2. Hot Jupiters that form beyond the major volatile (H2O/CO/CO2) ice lines and subsequently migrate post disk-dissipation are predicted have atmospheric carbon-to-oxygen ratios (C/O) near 1 and subsolar metallicities2, whereas planets that migrate through the disk before dissipation are predicted to be heavily polluted by infalling O-rich icy planetesimals, resulting in C/O

Date: 2021
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DOI: 10.1038/s41586-021-03912-6

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