Photochemical Hazes Dramatically Alter Temperature Structure and Atmospheric Circulation in 3D Simulations of Hot Jupiters
The Astrophysical Journal, vol. 951, pp. 117
Abstract
Abstract Photochemical hazes are expected to form in hot Jupiter atmospheres and may explain the strong scattering slopes and muted spectral features observed in the transmission spectra of many hot Jupiters. Absorption and scattering by photochemical hazes have the potential to drastically alter temperature structure and atmospheric circulation of these planets but have previously been neglected in general circulation models (GCMs). We present GCM simulations of the hot Jupiter HD 189733 b that include photochemical hazes as a radiatively active tracer fully coupled to atmospheric dynamics. The influence of haze radiative feedback strongly depends on the assumed haze optical properties. For soot hazes, two distinct thermal inversions form, separated by a local temperature minimum around 10−5 bar caused by upwelling on the dayside mixing air with low haze abundance upwards. The equatorial jet broadens and slows down. The horizontal distribution of hazes remains relatively similar to simulations with radiatively passive tracers. For Titan-type hazes, the equatorial jet accelerates and extends to much lower pressures, resulting in a dramatically different 3D distribution of hazes compared to radiatively passive or soot hazes. Further experimental and observational studies to constrain the optical properties of photochemical hazes will therefore be crucial for understanding the role of hazes in exoplanetary atmospheres. In the dayside emission spectrum, for both types of hazes the amplitude of near-infrared features is reduced, while the emitted flux at longer wavelengths (>4 μm) increases. Haze radiative feedback leads to increased phase-curve amplitudes in many infrared wavelength regions, mostly due to stronger dayside emission.
Authors 8
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Maria E. Steinrueck corresponding
University of Arizona · Max Planck Institute for Astronomy
Affiliation as printed
Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, 85721, USA
Max-Planck-Institut für Astronomie, D-69117 Heidelberg, Germany; steinrueck@mpia.de
Max-Planck-Institut für Astronomie, D-69117 Heidelberg, Germany
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Affiliation as printed
Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, 85721, USA
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Centre National de la Recherche Scientifique · Groupe de Spectrométrie Moléculaire et Atmosphérique · Université de Reims Champagne-Ardenne
Affiliation as printed
Groupe de spectrométrie moléculaire et atmosphérique, UMR CNRS 7331, Université de Reims Champagne Ardenne, 51687 Reims Cedex 2, Reims, France
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Centre National de la Recherche Scientifique · Université Côte d'Azur · University of Oxford · Lagrange Laboratory · Observatoire de la Côte d’Azur
Affiliation as printed
Atmospheric, Ocean, and Planetary Physics, Department of Physics, Oxford University, Oxford, OX1 3PU, UK
Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, France
Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, France
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Leiden University · Max Planck Institute for Astronomy · Leiden Observatory
Affiliation as printed
Leiden Observatory, Leiden University, Niels Bohrweg 2, 2333CA Leiden, The Netherlands
Max-Planck-Institut für Astronomie, D-69117 Heidelberg, Germany; steinrueck@mpia.de
Max-Planck-Institut für Astronomie, D-69117 Heidelberg, Germany
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Affiliation as printed
Atmospheric, Ocean, and Planetary Physics, Department of Physics, Oxford University, Oxford, OX1 3PU, UK
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University of California, Santa Cruz
Affiliation as printed
Department of Earth and Planetary Sciences, University of California Santa Cruz, Santa Cruz, CA 95064, USA
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Max Planck Institute for Astronomy
Affiliation as printed
Max-Planck-Institut für Astronomie, D-69117 Heidelberg, Germany; steinrueck@mpia.de
Max-Planck-Institut für Astronomie, D-69117 Heidelberg, Germany
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