Global Chemistry and Thermal Structure Models for the Hot Jupiter WASP-43b and Predictions for JWST. (arXiv:2001.04759v1 [astro-ph.EP])

Global Chemistry and Thermal Structure Models for the Hot Jupiter WASP-43b and Predictions for JWST. (arXiv:2001.04759v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Venot_O/0/1/0/all/0/1">Olivia Venot</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parmentier_V/0/1/0/all/0/1">Vivien Parmentier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blecic_J/0/1/0/all/0/1">Jasmina Blecic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cubillos_P/0/1/0/all/0/1">Patricio E. Cubillos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Waldmann_I/0/1/0/all/0/1">Ingo P. Waldmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Changeat_Q/0/1/0/all/0/1">Quentin Changeat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moses_J/0/1/0/all/0/1">Julianne I. Moses</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tremblin_P/0/1/0/all/0/1">Pascal Tremblin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crouzet_N/0/1/0/all/0/1">Nicolas Crouzet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gao_P/0/1/0/all/0/1">Peter Gao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Powell_D/0/1/0/all/0/1">Diana Powell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lagage_P/0/1/0/all/0/1">Pierre-Olivier Lagage</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dobbs_Dixon_I/0/1/0/all/0/1">Ian Dobbs-Dixon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Steinrueck_M/0/1/0/all/0/1">Maria E. Steinrueck</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kreidberg_L/0/1/0/all/0/1">Laura Kreidberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Batalha_N/0/1/0/all/0/1">Natalie Batalha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bean_J/0/1/0/all/0/1">Jacob L. Bean</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stevenson_K/0/1/0/all/0/1">Kevin B. Stevenson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Casewell_S/0/1/0/all/0/1">Sarah Casewell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carone_L/0/1/0/all/0/1">Ludmila Carone</a>

The James Webb Space Telescope (JWST) is expected to revolutionize the field
of exoplanets. The broad wavelength coverage and the high sensitivity of its
instruments will allow characterization of exoplanetary atmospheres with
unprecedented precision. Following the Call for the Cycle 1 Early Release
Science Program, the Transiting Exoplanet Community was awarded time to observe
several targets, including WASP-43b. The atmosphere of this hot Jupiter has
been intensively observed but still harbors some mysteries, especially
concerning the day-night temperature gradient, the efficiency of the
atmospheric circulation, and the presence of nightside clouds. We will
constrain these properties by observing a full orbit of the planet and
extracting its spectroscopic phase curve in the 5–12 $mu$m range with
JWST/MIRI. To prepare for these observations, we performed an extensive
modeling work with various codes: radiative transfer, chemical kinetics, cloud
microphysics, global circulation models, JWST simulators, and spectral
retrieval. Our JWST simulations show that we should achieve a precision of 210
ppm per 0.1 $mu$m spectral bin on average, which will allow us to measure the
variations of the spectrum in longitude and measure the night-side emission
spectrum for the first time. If the atmosphere of WASP-43b is clear, our
observations will permit us to determine if its atmosphere has an equilibrium
or disequilibrium chemical composition, providing eventually the first
conclusive evidence of chemical quenching in a hot Jupiter atmosphere. If the
atmosphere is cloudy, a careful retrieval analysis will allow us to identify
the cloud composition.

The James Webb Space Telescope (JWST) is expected to revolutionize the field
of exoplanets. The broad wavelength coverage and the high sensitivity of its
instruments will allow characterization of exoplanetary atmospheres with
unprecedented precision. Following the Call for the Cycle 1 Early Release
Science Program, the Transiting Exoplanet Community was awarded time to observe
several targets, including WASP-43b. The atmosphere of this hot Jupiter has
been intensively observed but still harbors some mysteries, especially
concerning the day-night temperature gradient, the efficiency of the
atmospheric circulation, and the presence of nightside clouds. We will
constrain these properties by observing a full orbit of the planet and
extracting its spectroscopic phase curve in the 5–12 $mu$m range with
JWST/MIRI. To prepare for these observations, we performed an extensive
modeling work with various codes: radiative transfer, chemical kinetics, cloud
microphysics, global circulation models, JWST simulators, and spectral
retrieval. Our JWST simulations show that we should achieve a precision of 210
ppm per 0.1 $mu$m spectral bin on average, which will allow us to measure the
variations of the spectrum in longitude and measure the night-side emission
spectrum for the first time. If the atmosphere of WASP-43b is clear, our
observations will permit us to determine if its atmosphere has an equilibrium
or disequilibrium chemical composition, providing eventually the first
conclusive evidence of chemical quenching in a hot Jupiter atmosphere. If the
atmosphere is cloudy, a careful retrieval analysis will allow us to identify
the cloud composition.

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