pub2019.bib
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@comment{{Command line: bib2bib -c 'not journal:"Discussions"' -c 'not title:"Correction to"' -c year=2019 -c $type="ARTICLE" -oc pub2019.txt -ob pub2019.bib leconte.link.bib}}
@article{2019ApJ...875...46Y,
author = {{Yang}, J. and {Leconte}, J. and {Wolf}, E.~T. and {Merlis}, T. and
{Koll}, D.~D.~B. and {Forget}, F. and {Abbot}, D.~S.},
title = {{Simulations of Water Vapor and Clouds on Rapidly Rotating and Tidally Locked Planets: A 3D Model Intercomparison}},
journal = {\apj},
keywords = {astrobiology, methods: numerical, planets and satellites: atmospheres, planets and satellites: general, radiative transfer },
year = 2019,
volume = 875,
eid = {46},
pages = {46},
abstract = {{Robustly modeling the inner edge of the habitable zone is essential for
determining the most promising potentially habitable exoplanets for
atmospheric characterization. Global climate models (GCMs) have become
the standard tool for calculating this boundary, but divergent results
have emerged among the various GCMs. In this study, we perform an
intercomparison of standard GCMs used in the field on a rapidly rotating
planet receiving a G-star spectral energy distribution and on a tidally
locked planet receiving an M-star spectral energy distribution.
Experiments both with and without clouds are examined. We find
relatively small difference (within 8 K) in global-mean surface
temperature simulation among the models in the G-star case with clouds.
In contrast, the global-mean surface temperature simulation in the
M-star case is highly divergent (20{\ndash}30 K). Moreover, even
differences in the simulated surface temperature when clouds are turned
off are significant. These differences are caused by differences in
cloud simulation and/or radiative transfer, as well as complex
interactions between atmospheric dynamics and these two processes. For
example we find that an increase in atmospheric absorption of shortwave
radiation can lead to higher relative humidity at high altitudes
globally and, therefore, a significant decrease in planetary radiation
emitted to space. This study emphasizes the importance of basing
conclusions about planetary climate on simulations from a variety of
GCMs and motivates the eventual comparison of GCM results with
terrestrial exoplanet observations to improve their performance.
}},
doi = {10.3847/1538-4357/ab09f1},
adsurl = {https://ui.adsabs.harvard.edu/abs/2019ApJ...875...46Y},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2019A&A...624A..17A,
author = {{Auclair-Desrotour}, P. and {Leconte}, J. and {Mergny}, C.},
title = {{Generic frequency dependence for the atmospheric tidal torque of terrestrial planets}},
journal = {\aap},
archiveprefix = {arXiv},
eprint = {1902.00280},
primaryclass = {astro-ph.EP},
keywords = {hydrodynamics, planet-star interactions, waves, planets and satellites: atmospheres},
year = 2019,
volume = 624,
eid = {A17},
pages = {A17},
abstract = {{Context. Thermal atmospheric tides have a strong impact on the rotation
of terrestrial planets. They can lock these planets into an asynchronous
rotation state of equilibrium.
Aims: We aim to characterize the
dependence of the tidal torque resulting from the semidiurnal thermal
tide on the tidal frequency, the planet orbital radius, and the
atmospheric surface pressure.
Methods: The tidal torque was
computed from full 3D simulations of the atmospheric climate and mean
flows using a generic version of the LMDZ general circulation model in
the case of a nitrogen-dominated atmosphere. Numerical results are
discussed with the help of an updated linear analytical framework. Power
scaling laws governing the evolution of the torque with the planet
orbital radius and surface pressure are derived.
Results: The
tidal torque exhibits (i) a thermal peak in the vicinity of
synchronization, (ii) a resonant peak associated with the excitation of
the Lamb mode in the high frequency range, and (iii) well defined
frequency slopes outside these resonances. These features are well
explained by our linear theory. Whatever the star-planet distance and
surface pressure, the torque frequency spectrum - when rescaled with the
relevant power laws - always presents the same behaviour. This allows us
to provide a single and easily usable empirical formula describing the
atmospheric tidal torque over the whole parameter space. With such a
formula, the effect of the atmospheric tidal torque can be implemented
in evolutionary models of the rotational dynamics of a planet in a
computationally efficient, and yet relatively accurate way.
}},
doi = {10.1051/0004-6361/201834685},
adsurl = {https://ui.adsabs.harvard.edu/abs/2019A%26A...624A..17A},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2019A&A...623A.161C,
author = {{Caldas}, A. and {Leconte}, J. and {Selsis}, F. and {Waldmann}, I.~P. and
{Bordé}, P. and {Rocchetto}, M. and {Charnay}, B.},
title = {{Effects of a fully 3D atmospheric structure on exoplanet transmission spectra: retrieval biases due to day-night temperature gradients}},
journal = {\aap},
archiveprefix = {arXiv},
eprint = {1901.09932},
primaryclass = {astro-ph.EP},
keywords = {planets and satellites: general, planets and satellites: atmospheres, radiative transfer, techniques: spectroscopic},
year = 2019,
volume = 623,
eid = {A161},
pages = {A161},
abstract = {{Transmission spectroscopy provides us with information on the
atmospheric properties at the limb, which is often intuitively assumed
to be a narrow annulus around the planet. Consequently, studies have
focused on the effect of atmospheric horizontal heterogeneities along
the limb. Here we demonstrate that the region probed in transmission -
the limb - actually extends significantly towards the day and night
sides of the planet. We show that the strong day-night thermal and
compositional gradients expected on synchronous exoplanets create
sufficient heterogeneities across the limb that result in important
systematic effects on the spectrum and bias its interpretation. To
quantify these effects, we developed a 3D radiative-transfer model able
to generate transmission spectra of atmospheres based on 3D atmospheric
structures. We first apply this tool to a simulation of the atmosphere
of GJ 1214 b to produce synthetic JWST observations and show that
producing a spectrum using only atmospheric columns at the terminator
results in errors greater than expected noise. This demonstrates the
necessity for a real 3D approach to model data for such precise
observatories. Secondly, we investigate how day-night temperature
gradients cause a systematic bias in retrieval analysis performed with
1D forward models. For that purpose we synthesise a large set of forward
spectra for prototypical HD 209458 b- and GJ 1214 b-type planets varying
the temperatures of the day and night sides as well as the width of the
transition region. We then perform typical retrieval analyses and
compare the retrieved parameters to the ground truth of the input model.
This study reveals systematic biases on the retrieved temperature (found
to be higher than the terminator temperature) and abundances. This is
due to the fact that the hotter dayside is more extended vertically and
screens the nightside - a result of the non-linear properties of
atmospheric transmission. These biases will be difficult to detect as
the 1D profiles used in the retrieval procedure are found to provide an
excellent match to the observed spectra based on standard fitting
criteria. This must be kept in mind when interpreting current and future
data.
}},
doi = {10.1051/0004-6361/201834384},
adsurl = {https://ui.adsabs.harvard.edu/abs/2019A%26A...623A.161C},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}