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A reflective, metal-rich atmosphere for GJ 1214b from its JWST phase curve.
Kempton, Eliza M-R; Zhang, Michael; Bean, Jacob L; Steinrueck, Maria E; Piette, Anjali A A; Parmentier, Vivien; Malsky, Isaac; Roman, Michael T; Rauscher, Emily; Gao, Peter; Bell, Taylor J; Xue, Qiao; Taylor, Jake; Savel, Arjun B; Arnold, Kenneth E; Nixon, Matthew C; Stevenson, Kevin B; Mansfield, Megan; Kendrew, Sarah; Zieba, Sebastian; Ducrot, Elsa; Dyrek, Achrène; Lagage, Pierre-Olivier; Stassun, Keivan G; Henry, Gregory W; Barman, Travis; Lupu, Roxana; Malik, Matej; Kataria, Tiffany; Ih, Jegug; Fu, Guangwei; Welbanks, Luis; McGill, Peter.
Afiliação
  • Kempton EM; Department of Astronomy, University of Maryland, College Park, MD, USA. ekempton@astro.umd.edu.
  • Zhang M; Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL, USA.
  • Bean JL; Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL, USA.
  • Steinrueck ME; Max-Planck Institute for Astronomy, Heidelberg, Germany.
  • Piette AAA; Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, USA.
  • Parmentier V; Department of Physics, University of Oxford, Oxford, UK.
  • Malsky I; Lagrange Laboratory, University of the Côte d'Azur, Observatory of the Côte d'Azur, CNRS, Nice, France.
  • Roman MT; Department of Astronomy, University of Michigan, Ann Arbor, MI, USA.
  • Rauscher E; School of Physics and Astronomy, University of Leicester, Leicester, UK.
  • Gao P; Department of Astronomy, University of Michigan, Ann Arbor, MI, USA.
  • Bell TJ; Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, USA.
  • Xue Q; BAER Institute, NASA Ames Research Center, Moffet Field, CA, USA.
  • Taylor J; Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL, USA.
  • Savel AB; Department of Physics, University of Oxford, Oxford, UK.
  • Arnold KE; Institut Trottier de Recherche sur les Exoplanètes and Department of Physics, University of Montréal, Montréal, Quebec, Canada.
  • Nixon MC; Department of Astronomy, University of Maryland, College Park, MD, USA.
  • Stevenson KB; Center for Computational Astrophysics, Flatiron Institute, New York, NY, USA.
  • Mansfield M; Department of Astronomy, University of Maryland, College Park, MD, USA.
  • Kendrew S; Department of Astronomy, University of Maryland, College Park, MD, USA.
  • Zieba S; Johns Hopkins Applied Physics Laboratory, Laurel, MD, USA.
  • Ducrot E; Steward Observatory, University of Arizona, Tucson, AZ, USA.
  • Dyrek A; European Space Agency, Space Telescope Science Institute, Baltimore, MD, USA.
  • Lagage PO; Max-Planck Institute for Astronomy, Heidelberg, Germany.
  • Stassun KG; Leiden Observatory, Leiden University, Leiden, the Netherlands.
  • Henry GW; Paris Region Fellow, Marie Sklodowska-Curie Action, Paris, France.
  • Barman T; AIM, CEA, CNRS, University of Paris-Saclay, University of Paris, Gif-sur-Yvette, France.
  • Lupu R; AIM, CEA, CNRS, University of Paris-Saclay, University of Paris, Gif-sur-Yvette, France.
  • Malik M; AIM, CEA, CNRS, University of Paris-Saclay, University of Paris, Gif-sur-Yvette, France.
  • Kataria T; Department of Physics and Astronomy, Vanderbilt University, Nashville, TN, USA.
  • Ih J; Center of Excellence in Information Systems, Tennessee State University, Nashville, TN, USA.
  • Fu G; Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA.
  • Welbanks L; Eureka Scientific, Inc., Oakland, CA, USA.
  • McGill P; Department of Astronomy, University of Maryland, College Park, MD, USA.
Nature ; 620(7972): 67-71, 2023 Aug.
Article em En | MEDLINE | ID: mdl-37164036
ABSTRACT
There are no planets intermediate in size between Earth and Neptune in our Solar System, yet these objects are found around a substantial fraction of other stars1. Population statistics show that close-in planets in this size range bifurcate into two classes on the basis of their radii2,3. It is proposed that the group with larger radii (referred to as 'sub-Neptunes') is distinguished by having hydrogen-dominated atmospheres that are a few percent of the total mass of the planets4. GJ 1214b is an archetype sub-Neptune that has been observed extensively using transmission spectroscopy to test this hypothesis5-14. However, the measured spectra are featureless, and thus inconclusive, due to the presence of high-altitude aerosols in the planet's atmosphere. Here we report a spectroscopic thermal phase curve of GJ 1214b obtained with the James Webb Space Telescope (JWST) in the mid-infrared. The dayside and nightside spectra (average brightness temperatures of 553 ± 9 and 437 ± 19 K, respectively) each show more than 3σ evidence of absorption features, with H2O as the most likely cause in both. The measured global thermal emission implies that GJ 1214b's Bond albedo is 0.51 ± 0.06. Comparison between the spectroscopic phase curve data and three-dimensional models of GJ 1214b reveal a planet with a high metallicity atmosphere blanketed by a thick and highly reflective layer of clouds or haze.
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Texto completo: 1 Coleções: 01-internacional Base de dados: MEDLINE Idioma: En Revista: Nature Ano de publicação: 2023 Tipo de documento: Article País de afiliação: Estados Unidos
Texto completo
Imprimir
XML
PubMed Links
Buscar no Google

Texto completo: 1 Coleções: 01-internacional Base de dados: MEDLINE Idioma: En Revista: Nature Ano de publicação: 2023 Tipo de documento: Article País de afiliação: Estados Unidos