pub2018.bib
@comment{{This file has been generated by bib2bib 1.96}}
@comment{{Command line: bib2bib -c 'not journal:"Discussions"' -c 'not title:"Correction to"' -c year=2018 -c $type="ARTICLE" -oc pub2018.txt -ob pub2018.bib leconte.link.bib}}
@article{2018PASP..130k4402B,
author = {{Bean}, J.~L. and {Stevenson}, K.~B. and {Batalha}, N.~M. and
{Berta-Thompson}, Z. and {Kreidberg}, L. and {Crouzet}, N. and
{Benneke}, B. and {Line}, M.~R. and {Sing}, D.~K. and {Wakeford}, H.~R. and
{Knutson}, H.~A. and {Kempton}, E.~M.-R. and {Désert}, J.-M. and
{Crossfield}, I. and {Batalha}, N.~E. and {de Wit}, J. and {Parmentier}, V. and
{Harrington}, J. and {Moses}, J.~I. and {Lopez-Morales}, M. and
{Alam}, M.~K. and {Blecic}, J. and {Bruno}, G. and {Carter}, A.~L. and
{Chapman}, J.~W. and {Decin}, L. and {Dragomir}, D. and {Evans}, T.~M. and
{Fortney}, J.~J. and {Fraine}, J.~D. and {Gao}, P. and {Garc{\'{\i}}a Mu{\~n}oz}, A. and
{Gibson}, N.~P. and {Goyal}, J.~M. and {Heng}, K. and {Hu}, R. and
{Kendrew}, S. and {Kilpatrick}, B.~M. and {Krick}, J. and {Lagage}, P.-O. and
{Lendl}, M. and {Louden}, T. and {Madhusudhan}, N. and {Mandell}, A.~M. and
{Mansfield}, M. and {May}, E.~M. and {Morello}, G. and {Morley}, C.~V. and
{Nikolov}, N. and {Redfield}, S. and {Roberts}, J.~E. and {Schlawin}, E. and
{Spake}, J.~J. and {Todorov}, K.~O. and {Tsiaras}, A. and {Venot}, O. and
{Waalkes}, W.~C. and {Wheatley}, P.~J. and {Zellem}, R.~T. and
{Angerhausen}, D. and {Barrado}, D. and {Carone}, L. and {Casewell}, S.~L. and
{Cubillos}, P.~E. and {Damiano}, M. and {de Val-Borro}, M. and
{Drummond}, B. and {Edwards}, B. and {Endl}, M. and {Espinoza}, N. and
{France}, K. and {Gizis}, J.~E. and {Greene}, T.~P. and {Henning}, T.~K. and
{Hong}, Y. and {Ingalls}, J.~G. and {Iro}, N. and {Irwin}, P.~G.~J. and
{Kataria}, T. and {Lahuis}, F. and {Leconte}, J. and {Lillo-Box}, J. and
{Lines}, S. and {Lothringer}, J.~D. and {Mancini}, L. and {Marchis}, F. and
{Mayne}, N. and {Palle}, E. and {Rauscher}, E. and {Roudier}, G. and
{Shkolnik}, E.~L. and {Southworth}, J. and {Swain}, M.~R. and
{Taylor}, J. and {Teske}, J. and {Tinetti}, G. and {Tremblin}, P. and
{Tucker}, G.~S. and {van Boekel}, R. and {Waldmann}, I.~P. and
{Weaver}, I.~C. and {Zingales}, T.},
title = {{The Transiting Exoplanet Community Early Release Science Program for JWST}},
journal = {\pasp},
archiveprefix = {arXiv},
eprint = {1803.04985},
primaryclass = {astro-ph.EP},
year = 2018,
volume = 130,
number = 11,
pages = {114402},
abstract = {{The James Webb Space Telescope (JWST) presents the opportunity to
transform our understanding of planets and the origins of life by
revealing the atmospheric compositions, structures, and dynamics of
transiting exoplanets in unprecedented detail. However, the
high-precision, timeseries observations required for such investigations
have unique technical challenges, and prior experience with Hubble,
Spitzer, and other facilities indicates that there will be a steep
learning curve when JWST becomes operational. In this paper, we describe
the science objectives and detailed plans of the Transiting Exoplanet
Community Early Release Science (ERS) Program, which is a recently
approved program for JWST observations early in Cycle 1. We also
describe the simulations used to establish the program. The goal of this
project, for which the obtained data will have no exclusive access
period, is to accelerate the acquisition and diffusion of technical
expertise for transiting exoplanet observations with JWST, while also
providing a compelling set of representative data sets that will enable
immediate scientific breakthroughs. The Transiting Exoplanet Community
ERS Program will exercise the timeseries modes of all four JWST
instruments that have been identified as the consensus highest
priorities, observe the full suite of transiting planet characterization
geometries (transits, eclipses, and phase curves), and target planets
with host stars that span an illustrative range of brightnesses. The
observations in this program were defined through an inclusive and
transparent process that had participation from JWST instrument experts
and international leaders in transiting exoplanet studies. The targets
have been vetted with previous measurements, will be observable early in
the mission, and have exceptional scientific merit. Community engagement
in the project will be centered on a two-phase Data Challenge that
culminates with the delivery of planetary spectra, timeseries instrument
performance reports, and open-source data analysis toolkits in time to
inform the agenda for Cycle 2 of the JWST mission.
}},
doi = {10.1088/1538-3873/aadbf3},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018PASP..130k4402B},
localpdf = {https://ui.adsabs.harvard.edu/abs/2018PASP..130k4402B.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2018ExA....46..211P,
author = {{Puig}, L. and {Pilbratt}, G. and {Heske}, A. and {Escudero}, I. and
{Crouzet}, P.-E. and {de Vogeleer}, B. and {Symonds}, K. and
{Kohley}, R. and {Drossart}, P. and {Eccleston}, P. and {Hartogh}, P. and
{Leconte}, J. and {Micela}, G. and {Ollivier}, M. and {Tinetti}, G. and
{Turrini}, D. and {Vandenbussche}, B. and {Wolkenberg}, P.},
title = {{The Phase A study of the ESA M4 mission candidate ARIEL}},
journal = {Experimental Astronomy},
keywords = {ARIEL, Cosmic vision, M4, ESA, Phase a study, Exoplanets, Transmission and eclipse spectroscopy},
year = 2018,
volume = 46,
pages = {211-239},
abstract = {{ARIEL, the Atmospheric Remote sensing Infrared Exoplanet Large survey,
is one of the three M-class mission candidates competing for the M4
launch slot within the Cosmic Vision science programme of the European
Space Agency (ESA). As such, ARIEL has been the subject of a Phase A
study that involved European industry, research institutes and
universities from ESA member states. This study is now completed and the
M4 down-selection is expected to be concluded in November 2017. ARIEL is
a concept for a dedicated mission to measure the chemical composition
and structure of hundreds of exoplanet atmospheres using the technique
of transit spectroscopy. ARIEL targets extend from gas giants (Jupiter
or Neptune-like) to super-Earths in the very hot to warm zones of F to
M-type host stars, opening up the way to large-scale, comparative
planetology that would place our own Solar System in the context of
other planetary systems in the Milky Way. A technical and programmatic
review of the ARIEL mission was performed between February and May 2017,
with the objective of assessing the readiness of the mission to progress
to the Phase B1 study. No critical issues were identified and the
mission was deemed technically feasible within the M4 programmatic
boundary conditions. In this paper we give an overview of the final
mission concept for ARIEL as of the end of the Phase A study, from
scientific, technical and operational perspectives.
}},
doi = {10.1007/s10686-018-9604-3},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018ExA....46..211P},
localpdf = {https://ui.adsabs.harvard.edu/abs/2018ExA....46..211P.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2018ExA....46..135T,
author = {{Tinetti}, G. and {Drossart}, P. and {Eccleston}, P. and {Hartogh}, P. and
{Heske}, A. and {Leconte}, J. and {Micela}, G. and {Ollivier}, M. and
{Pilbratt}, G. and {Puig}, L. and {Turrini}, D. and {Vandenbussche}, B. and
{Wolkenberg}, P. and {Beaulieu}, J.-P. and {Buchave}, L.~A. and
{Ferus}, M. and {Griffin}, M. and {Guedel}, M. and {Justtanont}, K. and
{Lagage}, P.-O. and {Machado}, P. and {Malaguti}, G. and {Min}, M. and
{N{\o}rgaard-Nielsen}, H.~U. and {Rataj}, M. and {Ray}, T. and
{Ribas}, I. and {Swain}, M. and {Szabo}, R. and {Werner}, S. and
{Barstow}, J. and {Burleigh}, M. and {Cho}, J. and {du Foresto}, V.~C. and
{Coustenis}, A. and {Decin}, L. and {Encrenaz}, T. and {Galand}, M. and
{Gillon}, M. and {Helled}, R. and {Morales}, J.~C. and {Mu{\~n}oz}, A.~G. and
{Moneti}, A. and {Pagano}, I. and {Pascale}, E. and {Piccioni}, G. and
{Pinfield}, D. and {Sarkar}, S. and {Selsis}, F. and {Tennyson}, J. and
{Triaud}, A. and {Venot}, O. and {Waldmann}, I. and {Waltham}, D. and
{Wright}, G. and {Amiaux}, J. and {Auguères}, J.-L. and
{Berthé}, M. and {Bezawada}, N. and {Bishop}, G. and {Bowles}, N. and
{Coffey}, D. and {Colomé}, J. and {Crook}, M. and {Crouzet}, P.-E. and
{Da Peppo}, V. and {Sanz}, I.~E. and {Focardi}, M. and {Frericks}, M. and
{Hunt}, T. and {Kohley}, R. and {Middleton}, K. and {Morgante}, G. and
{Ottensamer}, R. and {Pace}, E. and {Pearson}, C. and {Stamper}, R. and
{Symonds}, K. and {Rengel}, M. and {Renotte}, E. and {Ade}, P. and
{Affer}, L. and {Alard}, C. and {Allard}, N. and {Altieri}, F. and
{André}, Y. and {Arena}, C. and {Argyriou}, I. and {Aylward}, A. and
{Baccani}, C. and {Bakos}, G. and {Banaszkiewicz}, M. and {Barlow}, M. and
{Batista}, V. and {Bellucci}, G. and {Benatti}, S. and {Bernardi}, P. and
{Bézard}, B. and {Blecka}, M. and {Bolmont}, E. and {Bonfond}, B. and
{Bonito}, R. and {Bonomo}, A.~S. and {Brucato}, J.~R. and {Brun}, A.~S. and
{Bryson}, I. and {Bujwan}, W. and {Casewell}, S. and {Charnay}, B. and
{Pestellini}, C.~C. and {Chen}, G. and {Ciaravella}, A. and
{Claudi}, R. and {Clédassou}, R. and {Damasso}, M. and {Damiano}, M. and
{Danielski}, C. and {Deroo}, P. and {Di Giorgio}, A.~M. and
{Dominik}, C. and {Doublier}, V. and {Doyle}, S. and {Doyon}, R. and
{Drummond}, B. and {Duong}, B. and {Eales}, S. and {Edwards}, B. and
{Farina}, M. and {Flaccomio}, E. and {Fletcher}, L. and {Forget}, F. and
{Fossey}, S. and {Fr{\"a}nz}, M. and {Fujii}, Y. and {Garc{\'{\i}}a-Piquer}, {\'A}. and
{Gear}, W. and {Geoffray}, H. and {Gérard}, J.~C. and {Gesa}, L. and
{Gomez}, H. and {Graczyk}, R. and {Griffith}, C. and {Grodent}, D. and
{Guarcello}, M.~G. and {Gustin}, J. and {Hamano}, K. and {Hargrave}, P. and
{Hello}, Y. and {Heng}, K. and {Herrero}, E. and {Hornstrup}, A. and
{Hubert}, B. and {Ida}, S. and {Ikoma}, M. and {Iro}, N. and
{Irwin}, P. and {Jarchow}, C. and {Jaubert}, J. and {Jones}, H. and
{Julien}, Q. and {Kameda}, S. and {Kerschbaum}, F. and {Kervella}, P. and
{Koskinen}, T. and {Krijger}, M. and {Krupp}, N. and {Lafarga}, M. and
{Landini}, F. and {Lellouch}, E. and {Leto}, G. and {Luntzer}, A. and
{Rank-L{\"u}ftinger}, T. and {Maggio}, A. and {Maldonado}, J. and
{Maillard}, J.-P. and {Mall}, U. and {Marquette}, J.-B. and
{Mathis}, S. and {Maxted}, P. and {Matsuo}, T. and {Medvedev}, A. and
{Miguel}, Y. and {Minier}, V. and {Morello}, G. and {Mura}, A. and
{Narita}, N. and {Nascimbeni}, V. and {Nguyen Tong}, N. and
{Noce}, V. and {Oliva}, F. and {Palle}, E. and {Palmer}, P. and
{Pancrazzi}, M. and {Papageorgiou}, A. and {Parmentier}, V. and
{Perger}, M. and {Petralia}, A. and {Pezzuto}, S. and {Pierrehumbert}, R. and
{Pillitteri}, I. and {Piotto}, G. and {Pisano}, G. and {Prisinzano}, L. and
{Radioti}, A. and {Réess}, J.-M. and {Rezac}, L. and {Rocchetto}, M. and
{Rosich}, A. and {Sanna}, N. and {Santerne}, A. and {Savini}, G. and
{Scandariato}, G. and {Sicardy}, B. and {Sierra}, C. and {Sindoni}, G. and
{Skup}, K. and {Snellen}, I. and {Sobiecki}, M. and {Soret}, L. and
{Sozzetti}, A. and {Stiepen}, A. and {Strugarek}, A. and {Taylor}, J. and
{Taylor}, W. and {Terenzi}, L. and {Tessenyi}, M. and {Tsiaras}, A. and
{Tucker}, C. and {Valencia}, D. and {Vasisht}, G. and {Vazan}, A. and
{Vilardell}, F. and {Vinatier}, S. and {Viti}, S. and {Waters}, R. and
{Wawer}, P. and {Wawrzaszek}, A. and {Whitworth}, A. and {Yung}, Y.~L. and
{Yurchenko}, S.~N. and {Osorio}, M.~R.~Z. and {Zellem}, R. and
{Zingales}, T. and {Zwart}, F.},
title = {{A chemical survey of exoplanets with ARIEL}},
journal = {Experimental Astronomy},
keywords = {Exoplanets, Space missions, IR spectroscopy, Molecular signatures},
year = 2018,
volume = 46,
pages = {135-209},
abstract = {{Thousands of exoplanets have now been discovered with a huge range of
masses, sizes and orbits: from rocky Earth-like planets to large gas
giants grazing the surface of their host star. However, the essential
nature of these exoplanets remains largely mysterious: there is no
known, discernible pattern linking the presence, size, or orbital
parameters of a planet to the nature of its parent star. We have little
idea whether the chemistry of a planet is linked to its formation
environment, or whether the type of host star drives the physics and
chemistry of the planet's birth, and evolution. ARIEL was conceived to
observe a large number ( 1000) of transiting planets for statistical
understanding, including gas giants, Neptunes, super-Earths and
Earth-size planets around a range of host star types using transit
spectroscopy in the 1.25-7.8 {$\mu$}m spectral range and multiple
narrow-band photometry in the optical. ARIEL will focus on warm and hot
planets to take advantage of their well-mixed atmospheres which should
show minimal condensation and sequestration of high-Z materials compared
to their colder Solar System siblings. Said warm and hot atmospheres are
expected to be more representative of the planetary bulk composition.
Observations of these warm/hot exoplanets, and in particular of their
elemental composition (especially C, O, N, S, Si), will allow the
understanding of the early stages of planetary and atmospheric formation
during the nebular phase and the following few million years. ARIEL will
thus provide a representative picture of the chemical nature of the
exoplanets and relate this directly to the type and chemical environment
of the host star. ARIEL is designed as a dedicated survey mission for
combined-light spectroscopy, capable of observing a large and
well-defined planet sample within its 4-year mission lifetime. Transit,
eclipse and phase-curve spectroscopy methods, whereby the signal from
the star and planet are differentiated using knowledge of the planetary
ephemerides, allow us to measure atmospheric signals from the planet at
levels of 10-100 part per million (ppm) relative to the star and, given
the bright nature of targets, also allows more sophisticated techniques,
such as eclipse mapping, to give a deeper insight into the nature of the
atmosphere. These types of observations require a stable payload and
satellite platform with broad, instantaneous wavelength coverage to
detect many molecular species, probe the thermal structure, identify
clouds and monitor the stellar activity. The wavelength range proposed
covers all the expected major atmospheric gases from e.g.
H$_{2}$O, CO$_{2}$, CH$_{4}$ NH$_{3}$, HCN,
H$_{2}$S through to the more exotic metallic compounds, such as
TiO, VO, and condensed species. Simulations of ARIEL performance in
conducting exoplanet surveys have been performed - using conservative
estimates of mission performance and a full model of all significant
noise sources in the measurement - using a list of potential ARIEL
targets that incorporates the latest available exoplanet statistics. The
conclusion at the end of the Phase A study, is that ARIEL - in line with
the stated mission objectives - will be able to observe about 1000
exoplanets depending on the details of the adopted survey strategy, thus
confirming the feasibility of the main science objectives.
}},
doi = {10.1007/s10686-018-9598-x},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018ExA....46..135T},
localpdf = {https://ui.adsabs.harvard.edu/abs/2018ExA....46..135T.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2018ExA....46...67Z,
author = {{Zingales}, T. and {Tinetti}, G. and {Pillitteri}, I. and {Leconte}, J. and
{Micela}, G. and {Sarkar}, S.},
title = {{The ARIEL mission reference sample}},
journal = {Experimental Astronomy},
archiveprefix = {arXiv},
eprint = {1706.08444},
primaryclass = {astro-ph.EP},
keywords = {Exoplanets, ARIEL space mission, Planetary population},
year = 2018,
volume = 46,
pages = {67-100},
abstract = {{The ARIEL (Atmospheric Remote-sensing Exoplanet Large-survey) mission
concept is one of the three M4 mission candidates selected by the
European Space Agency (ESA) for a Phase A study, competing for a launch
in 2026. ARIEL has been designed to study the physical and chemical
properties of a large and diverse sample of exoplanets and, through
those, understand how planets form and evolve in our galaxy. Here we
describe the assumptions made to estimate an optimal sample of
exoplanets - including already known exoplanets and expected ones yet to
be discovered - observable by ARIEL and define a realistic mission
scenario. To achieve the mission objectives, the sample should include
gaseous and rocky planets with a range of temperatures around stars of
different spectral type and metallicity. The current ARIEL design
enables the observation of {\tilde}1000 planets, covering a broad range
of planetary and stellar parameters, during its four year mission
lifetime. This nominal list of planets is expected to evolve over the
years depending on the new exoplanet discoveries.
}},
doi = {10.1007/s10686-018-9572-7},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018ExA....46...67Z},
localpdf = {https://ui.adsabs.harvard.edu/abs/2018ExA....46...67Z.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2018ExA....46...45T,
author = {{Turrini}, D. and {Miguel}, Y. and {Zingales}, T. and {Piccialli}, A. and
{Helled}, R. and {Vazan}, A. and {Oliva}, F. and {Sindoni}, G. and
{Pani{\'c}}, O. and {Leconte}, J. and {Min}, M. and {Pirani}, S. and
{Selsis}, F. and {Coudé du Foresto}, V. and {Mura}, A. and
{Wolkenberg}, P.},
title = {{The contribution of the ARIEL space mission to the study of planetary formation}},
journal = {Experimental Astronomy},
archiveprefix = {arXiv},
eprint = {1804.06179},
primaryclass = {astro-ph.EP},
keywords = {Atmospheric remote-sensing infrared exoplanet large-survey, ARIEL, Space missions, Exoplanets, Planetary formation, Astrochemistry},
year = 2018,
volume = 46,
pages = {45-65},
abstract = {{The study of extrasolar planets and of the Solar System provides
complementary pieces of the mosaic represented by the process of
planetary formation. Exoplanets are essential to fully grasp the huge
diversity of outcomes that planetary formation and the subsequent
evolution of the planetary systems can produce. The orbital and basic
physical data we currently possess for the bulk of the exoplanetary
population, however, do not provide enough information to break the
intrinsic degeneracy of their histories, as different evolutionary
tracks can result in the same final configurations. The lessons learned
from the Solar System indicate us that the solution to this problem lies
in the information contained in the composition of planets. The goal of
the Atmospheric Remote-Sensing Infrared Exoplanet Large-survey (ARIEL),
one of the three candidates as ESA M4 space mission, is to observe a
large and diversified population of transiting planets around a range of
host star types to collect information on their atmospheric composition.
ARIEL will focus on warm and hot planets to take advantage of their
well-mixed atmospheres, which should show minimal condensation and
sequestration of high-Z materials and thus reveal their bulk composition
across all main cosmochemical elements. In this work we will review the
most outstanding open questions concerning the way planets form and the
mechanisms that contribute to create habitable environments that the
compositional information gathered by ARIEL will allow to tackle.
}},
doi = {10.1007/s10686-017-9570-1},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018ExA....46...45T},
localpdf = {https://ui.adsabs.harvard.edu/abs/2018ExA....46...45T.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2018AJ....156..218D,
author = {{Ducrot}, E. and {Sestovic}, M. and {Morris}, B.~M. and {Gillon}, M. and
{Triaud}, A.~H.~M.~J. and {De Wit}, J. and {Thimmarayappa}, D. and
{Agol}, E. and {Almleaky}, Y. and {Burdanov}, A. and {Burgasser}, A.~J. and
{Delrez}, L. and {Demory}, B.-O. and {Jehin}, E. and {Leconte}, J. and
{McCormac}, J. and {Murray}, C. and {Queloz}, D. and {Selsis}, F. and
{Thompson}, S. and {Van Grootel}, V.},
title = {{The 0.8-4.5 {$\mu$}m Broadband Transmission Spectra of TRAPPIST-1 Planets}},
journal = {\aj},
archiveprefix = {arXiv},
eprint = {1807.01402},
primaryclass = {astro-ph.EP},
keywords = {binaries: eclipsing, planetary systems, techniques: photometric, techniques: spectroscopic},
year = 2018,
volume = 156,
eid = {218},
pages = {218},
abstract = {{The TRAPPIST-1 planetary system provides an exceptional opportunity for
the atmospheric characterization of temperate terrestrial exoplanets
with the upcoming James Webb Space Telescope (JWST). Assessing the
potential impact of stellar contamination on the planets{\rsquo} transit
transmission spectra is an essential precursor to this characterization.
Planetary transits themselves can be used to scan the stellar
photosphere and to constrain its heterogeneity through transit depth
variations in time and wavelength. In this context, we present our
analysis of 169 transits observed in the optical from space with K2 and
from the ground with the SPECULOOS and Liverpool telescopes. Combining
our measured transit depths with literature results gathered in the
mid-/near-IR with Spitzer/IRAC and HST/WFC3, we construct the broadband
transmission spectra of the TRAPPIST-1 planets over the 0.8-4.5
{$\mu$}m spectral range. While planet b, d, and f spectra show some
structures at the 200-300 ppm level, the four others are globally
flat. Even if we cannot discard their instrumental origins, two
scenarios seem to be favored by the data: a stellar photosphere
dominated by a few high-latitude giant (cold) spots, or, alternatively,
by a few small and hot (3500-4000 K) faculae. In both cases, the
stellar contamination of the transit transmission spectra is expected to
be less dramatic than predicted in recent papers. Nevertheless, based on
our results, stellar contamination can still be of comparable or greater
order than planetary atmospheric signals at certain wavelengths.
Understanding and correcting the effects of stellar heterogeneity
therefore appears essential for preparing for the exploration of
TRAPPIST-1 with JWST.
}},
doi = {10.3847/1538-3881/aade94},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018AJ....156..218D},
localpdf = {https://ui.adsabs.harvard.edu/abs/2018AJ....156..218D.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2018A&A...615A..23A,
author = {{Auclair-Desrotour}, P. and {Mathis}, S. and {Laskar}, J. and
{Leconte}, J.},
title = {{Oceanic tides from Earth-like to ocean planets}},
journal = {\aap},
archiveprefix = {arXiv},
eprint = {1801.08742},
primaryclass = {astro-ph.EP},
keywords = {hydrodynamics, planet-star interactions, planets and satellites: oceans, planets and satellites: terrestrial planets},
year = 2018,
volume = 615,
eid = {A23},
pages = {A23},
abstract = {{Context. Oceanic tides are a major source of tidal dissipation. They
drive the evolution of planetary systems and the rotational dynamics of
planets. However, two-dimensional (2D) models commonly used for the
Earth cannot be applied to extrasolar telluric planets hosting
potentially deep oceans because they ignore the three-dimensional (3D)
effects related to the ocean's vertical structure.
Aims: Our goal
is to investigate, in a consistant way, the importance of the
contribution of internal gravity waves in the oceanic tidal response and
to propose a modelling that allows one to treat a wide range of cases
from shallow to deep oceans.
Methods: A 3D ab initio model is
developed to study the dynamics of a global planetary ocean. This model
takes into account compressibility, stratification, and sphericity
terms, which are usually ignored in 2D approaches. An analytic solution
is computed and used to study the dependence of the tidal response on
the tidal frequency and on the ocean depth and stratification.
Results: In the 2D asymptotic limit, we recover the frequency-resonant
behaviour due to surface inertial-gravity waves identified by early
studies. As the ocean depth and Brunt-V{\"a}is{\"a}l{\"a} frequency
increase, the contribution of internal gravity waves grows in importance
and the tidal response becomes 3D. In the case of deep oceans, the
stable stratification induces resonances that can increase the tidal
dissipation rate by several orders of magnitude. It is thus able to
significantly affect the evolution time scale of the planetary rotation.
}},
doi = {10.1051/0004-6361/201732249},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018A%26A...615A..23A},
localpdf = {https://ui.adsabs.harvard.edu/abs/2018A_26A...615A..23A.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2018A&A...613A..68G,
author = {{Grimm}, S.~L. and {Demory}, B.-O. and {Gillon}, M. and {Dorn}, C. and
{Agol}, E. and {Burdanov}, A. and {Delrez}, L. and {Sestovic}, M. and
{Triaud}, A.~H.~M.~J. and {Turbet}, M. and {Bolmont}, {\'E}. and
{Caldas}, A. and {de Wit}, J. and {Jehin}, E. and {Leconte}, J. and
{Raymond}, S.~N. and {Van Grootel}, V. and {Burgasser}, A.~J. and
{Carey}, S. and {Fabrycky}, D. and {Heng}, K. and {Hernandez}, D.~M. and
{Ingalls}, J.~G. and {Lederer}, S. and {Selsis}, F. and {Queloz}, D.
},
title = {{The nature of the TRAPPIST-1 exoplanets}},
journal = {\aap},
archiveprefix = {arXiv},
eprint = {1802.01377},
primaryclass = {astro-ph.EP},
keywords = {methods: numerical, planets and satellites: detection, planets and satellites: individual: TRAPPIST-1},
year = 2018,
volume = 613,
eid = {A68},
pages = {A68},
abstract = {{Context. The TRAPPIST-1 system hosts seven Earth-sized, temperate
exoplanets orbiting an ultra-cool dwarf star. As such, it represents a
remarkable setting to study the formation and evolution of terrestrial
planets that formed in the same protoplanetary disk. While the sizes of
the TRAPPIST-1 planets are all known to better than 5\% precision, their
densities have significant uncertainties (between 28\% and 95\%) because
of poor constraints on the planet's masses.
Aims: The goal of
this paper is to improve our knowledge of the TRAPPIST-1 planetary
masses and densities using transit-timing variations (TTVs). The
complexity of the TTV inversion problem is known to be particularly
acute in multi-planetary systems (convergence issues, degeneracies and
size of the parameter space), especially for resonant chain systems such
as TRAPPIST-1.
Methods: To overcome these challenges, we have
used a novel method that employs a genetic algorithm coupled to a full
N-body integrator that we applied to a set of 284 individual transit
timings. This approach enables us to efficiently explore the parameter
space and to derive reliable masses and densities from TTVs for all
seven planets.
Results: Our new masses result in a five- to
eight-fold improvement on the planetary density uncertainties, with
precisions ranging from 5\% to 12\%. These updated values provide new
insights into the bulk structure of the TRAPPIST-1 planets. We find that
TRAPPIST-1 c and e likely have largely rocky interiors, while planets b,
d, f, g, and h require envelopes of volatiles in the form of thick
atmospheres, oceans, or ice, in most cases with water mass fractions
less than 5\%.
}},
doi = {10.1051/0004-6361/201732233},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018A%26A...613A..68G},
localpdf = {https://ui.adsabs.harvard.edu/abs/2018A_26A...613A..68G.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2018A&A...613A..45A,
author = {{Auclair-Desrotour}, P. and {Leconte}, J.},
title = {{Semidiurnal thermal tides in asynchronously rotating hot Jupiters}},
journal = {\aap},
archiveprefix = {arXiv},
eprint = {1801.07519},
primaryclass = {astro-ph.EP},
keywords = {hydrodynamics, planet-star interactions, waves, planets and satellites: atmospheres, planets and satellites: gaseous planets},
year = 2018,
volume = 613,
eid = {A45},
pages = {A45},
abstract = {{Context. Thermal tides can torque the atmosphere of hot Jupiters into
asynchronous rotation, while these planets are usually assumed to be
locked into spin-orbit synchronization with their host star.
Aims: In this work, our goal is to characterize the tidal response of a
rotating hot Jupiter to the tidal semidiurnal thermal forcing of its
host star by identifying the structure of tidal waves responsible for
variation of mass distribution, their dependence on the tidal frequency,
and their ability to generate strong zonal flows.
Methods: We
develop an ab initio global modelling that generalizes the early
approach of Arras {\amp} Socrates (2010, ApJ, 714, 1) to rotating and
non-adiabatic planets. We analytically derive the torque exerted on the
body and the associated timescales of evolution, as well as the
equilibrium tidal response of the atmosphere in the zero-frequency
limit. Finally, we numerically integrate the equations of thermal tides
for three cases, including dissipation and rotation step by step.
Results: The resonances associated with tidally generated
gravito-inertial waves significantly amplify the resulting tidal torque
in the range 1-30 days. This torque can globally drive the atmosphere
into asynchronous rotation, as its sign depends on the tidal frequency.
The resonant behaviour of the tidal response is enhanced by rotation,
which couples the forcing to several Hough modes in the general case,
while the radiative cooling tends to regularize it and diminish its
amplitude.
}},
doi = {10.1051/0004-6361/201731683},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018A%26A...613A..45A},
localpdf = {https://ui.adsabs.harvard.edu/abs/2018A_26A...613A..45A.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2018A&A...612A..86T,
author = {{Turbet}, M. and {Bolmont}, E. and {Leconte}, J. and {Forget}, F. and
{Selsis}, F. and {Tobie}, G. and {Caldas}, A. and {Naar}, J. and
{Gillon}, M.},
title = {{Modeling climate diversity, tidal dynamics and the fate of volatiles on TRAPPIST-1 planets}},
journal = {\aap},
archiveprefix = {arXiv},
eprint = {1707.06927},
primaryclass = {astro-ph.EP},
keywords = {stars: individual: TRAPPIST-1, planets and satellites: terrestrial planets, planets and satellites: atmospheres, planets and satellites: dynamical evolution and stability, astrobiology},
year = 2018,
volume = 612,
eid = {A86},
pages = {A86},
abstract = {{TRAPPIST-1 planets are invaluable for the study of comparative planetary
science outside our solar system and possibly habitability. Both transit
timing variations (TTV) of the planets and the compact, resonant
architecture of the system suggest that TRAPPIST-1 planets could be
endowed with various volatiles today. First, we derived from N-body
simulations possible planetary evolution scenarios, and show that all
the planets are likely in synchronous rotation. We then used a versatile
3D global climate model (GCM) to explore the possible climates of cool
planets around cool stars, with a focus on the TRAPPIST-1 system. We
investigated the conditions required for cool planets to prevent
possible volatile species to be lost permanently by surface
condensation, irreversible burying or photochemical destruction. We also
explored the resilience of the same volatiles (when in condensed phase)
to a runaway greenhouse process. We find that background atmospheres
made of N$_{2}$, CO, or O$_{2}$ are rather resistant to
atmospheric collapse. However, even if TRAPPIST-1 planets were able to
sustain a thick background atmosphere by surviving early X/EUV radiation
and stellar wind atmospheric erosion, it is difficult for them to
accumulate significant greenhouse gases like CO$_{2}$,
CH$_{4}$, or NH$_{3}$. CO$_{2}$ can easily condense on
the permanent nightside, forming CO$_{2}$ ice glaciers that would
flow toward the substellar region. A complete CO$_{2}$ ice surface
cover is theoretically possible on TRAPPIST-1g and h only, but
CO$_{2}$ ices should be gravitationally unstable and get buried
beneath the water ice shell in geologically short timescales. Given
TRAPPIST-1 planets large EUV irradiation (at least 10$^{3}$
{\times} Titan's flux), CH$_{4}$ and NH$_{3}$ are
photodissociated rapidly and are thus hard to accumulate in the
atmosphere. Photochemical hazes could then sedimentate and form a
surface layer of tholins that would progressively thicken over the age
of the TRAPPIST-1 system. Regarding habitability, we confirm that few
bars of CO$_{2}$ would suffice to warm the surface of TRAPPIST-1f
and g above the melting point of water. We also show that TRAPPIST-1e is
a remarkable candidate for surface habitability. If the planet is today
synchronous and abundant in water, then it should very likely sustain
surface liquid water at least in the substellar region, whatever the
atmosphere considered.
}},
doi = {10.1051/0004-6361/201731620},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018A%26A...612A..86T},
localpdf = {https://ui.adsabs.harvard.edu/abs/2018A_26A...612A..86T.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2018MNRAS.475.3577D,
author = {{Delrez}, L. and {Gillon}, M. and {Triaud}, A.~H.~M.~J. and
{Demory}, B.-O. and {de Wit}, J. and {Ingalls}, J.~G. and {Agol}, E. and
{Bolmont}, E. and {Burdanov}, A. and {Burgasser}, A.~J. and
{Carey}, S.~J. and {Jehin}, E. and {Leconte}, J. and {Lederer}, S. and
{Queloz}, D. and {Selsis}, F. and {Van Grootel}, V.},
title = {{Early 2017 observations of TRAPPIST-1 with Spitzer}},
journal = {\mnras},
archiveprefix = {arXiv},
eprint = {1801.02554},
primaryclass = {astro-ph.EP},
keywords = {techniques: photometric, stars: individual: TRAPPIST-1, planetary systems},
year = 2018,
volume = 475,
pages = {3577-3597},
abstract = {{The recently detected TRAPPIST-1 planetary system, with its seven
planets transiting a nearby ultracool dwarf star, offers the first
opportunity to perform comparative exoplanetology of temperate
Earth-sized worlds. To further advance our understanding of these
planets' compositions, energy budgets, and dynamics, we are carrying out
an intensive photometric monitoring campaign of their transits with the
Spitzer Space Telescope. In this context, we present 60 new transits of
the TRAPPIST-1 planets observed with Spitzer/Infrared Array Camera
(IRAC) in 2017 February and March. We combine these observations with
previously published Spitzer transit photometry and perform a global
analysis of the resulting extensive data set. This analysis refines the
transit parameters and provides revised values for the planets' physical
parameters, notably their radii, using updated properties for the star.
As part of our study, we also measure precise transit timings that will
be used in a companion paper to refine the planets' masses and
compositions using the transit timing variations method. TRAPPIST-1
shows a very low level of low-frequency variability in the IRAC
4.5-{$\mu$}m band, with a photometric RMS of only 0.11 per cent at a 123-s
cadence. We do not detect any evidence of a (quasi-)periodic signal
related to stellar rotation. We also analyse the transit light curves
individually, to search for possible variations in the transit
parameters of each planet due to stellar variability, and find that the
Spitzer transits of the planets are mostly immune to the effects of
stellar variations. These results are encouraging for forthcoming
transmission spectroscopy observations of the TRAPPIST-1 planets with
the James Webb Space Telescope.
}},
doi = {10.1093/mnras/sty051},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018MNRAS.475.3577D},
localpdf = {https://ui.adsabs.harvard.edu/abs/2018MNRAS.475.3577D.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2018NatAs...2..214D,
author = {{de Wit}, J. and {Wakeford}, H.~R. and {Lewis}, N.~K. and {Delrez}, L. and
{Gillon}, M. and {Selsis}, F. and {Leconte}, J. and {Demory}, B.-O. and
{Bolmont}, E. and {Bourrier}, V. and {Burgasser}, A.~J. and
{Grimm}, S. and {Jehin}, E. and {Lederer}, S.~M. and {Owen}, J.~E. and
{Stamenkovi{\'c}}, V. and {Triaud}, A.~H.~M.~J.},
title = {{Atmospheric reconnaissance of the habitable-zone Earth-sized planets orbiting TRAPPIST-1}},
journal = {Nature Astronomy},
archiveprefix = {arXiv},
eprint = {1802.02250},
primaryclass = {astro-ph.EP},
year = 2018,
volume = 2,
pages = {214-219},
abstract = {{Seven temperate Earth-sized exoplanets readily amenable for atmospheric
studies transit the nearby ultracool dwarf star TRAPPIST-1 (refs
$^{1,2}$). Their atmospheric regime is unknown and could range
from extended primordial hydrogen-dominated to depleted
atmospheres$^{3-6}$. Hydrogen in particular is a powerful
greenhouse gas that may prevent the habitability of inner planets while
enabling the habitability of outer ones$^{6-8}$. An atmosphere
largely dominated by hydrogen, if cloud-free, should yield prominent
spectroscopic signatures in the near-infrared detectable during
transits. Observations of the innermost planets have ruled out such
signatures$^{9}$. However, the outermost planets are more likely
to have sustained such a Neptune-like atmosphere$^{10, 11}$. Here,
we report observations for the four planets within or near the system's
habitable zone, the circumstellar region where liquid water could exist
on a planetary surface$^{12-14}$. These planets do not exhibit
prominent spectroscopic signatures at near-infrared wavelengths either,
which rules out cloud-free hydrogen-dominated atmospheres for TRAPPIST-1
d, e and f, with significance of 8{$\sigma$}, 6{$\sigma$} and 4{$\sigma$},
respectively. Such an atmosphere is instead not excluded for planet g.
As high-altitude clouds and hazes are not expected in hydrogen-dominated
atmospheres around planets with such insolation$^{15, 16}$, these
observations further support their terrestrial and potentially habitable
nature.
}},
doi = {10.1038/s41550-017-0374-z},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018NatAs...2..214D},
localpdf = {https://ui.adsabs.harvard.edu/abs/2018NatAs...2..214D.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2018NatGe..11..168L,
author = {{Leconte}, J.},
title = {{Continuous reorientation of synchronous terrestrial planets due to mantle convection}},
journal = {Nature Geoscience},
archiveprefix = {arXiv},
eprint = {1809.01150},
primaryclass = {astro-ph.EP},
year = 2018,
volume = 11,
pages = {168-172},
abstract = {{Many known rocky exoplanets are thought to have been spun down by tidal
interactions to a state of synchronous rotation, in which a planet's
period of rotation is equal to that of its orbit around its host star.
Investigations into atmospheric and surface processes occurring on such
exoplanets thus commonly assume that day and night sides are fixed with
respect to the surface over geological timescales. Here we use an
analytical model to show that true polar wander{\mdash}where a planetary
body's spin axis shifts relative to its surface because of changes in
mass distribution{\mdash}can continuously reorient a synchronous rocky
exoplanet. As occurs on Earth, we find that even weak mantle convection
in a rocky exoplanet can produce density heterogeneities within the
mantle sufficient to reorient the planet. Moreover, we show that this
reorientation is made very efficient by the slower rotation rate of a
synchronous planet when compared with Earth, which limits the
stabilizing effect of rotational and tidal deformations. Furthermore, a
relatively weak lithosphere limits its ability to support remnant loads
and stabilize against reorientation. Although uncertainties exist
regarding the mantle and lithospheric evolution of these worlds, we
suggest that the axes of smallest and largest moment of inertia of
synchronous exoplanets with active mantle convection change continuously
over time, but remain closely aligned with the star-planet and orbital
axes, respectively.
}},
doi = {10.1038/s41561-018-0071-2},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018NatGe..11..168L},
localpdf = {https://ui.adsabs.harvard.edu/abs/2018NatGe..11..168L.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2018ApJ...853L..30L,
author = {{Leconte}, J.},
title = {{Why Compositional Convection Cannot Explain Substellar Objects{\rsquo} Sharp Spectral-type Transitions}},
journal = {\apjl},
archiveprefix = {arXiv},
eprint = {1801.08142},
primaryclass = {astro-ph.SR},
keywords = {brown dwarfs, hydrodynamics, planets and satellites: atmospheres, planets and satellites: gaseous planets},
year = 2018,
volume = 853,
eid = {L30},
pages = {L30},
abstract = {{As brown dwarfs and young giant planets cool down, they are known to
experience various chemical transitions{\mdash}for example, from $\{$CO$\}$
rich L-dwarfs to methane rich T-dwarfs. Those chemical transitions are
accompanied by spectral transitions with sharpness that cannot be
explained by chemistry alone. In a series of articles, Tremblin et al.
proposed that some of the yet-unexplained features associated with these
transitions could be explained by a reduction of the thermal gradient
near the photosphere. To explain, in turn, this more isothermal profile,
they invoke the presence of an instability analogous to fingering
convection{\mdash}compositional convection{\mdash}triggered by the change
in mean molecular weight of the gas due to the chemical transitions
mentioned above. In this Letter, we use existing arguments to
demonstrate that any turbulent transport, if present, would in fact
increase the thermal gradient. This misinterpretation comes from the
fact that turbulence mixes/homogenizes entropy (potential temperature)
instead of temperature. So, while increasing transport, turbulence in an
initially stratified atmosphere actually carries energy downward,
whether it is due to fingering or any other type of compositional
convection. These processes therefore cannot explain the features
observed along the aforementioned transitions by reducing the thermal
gradient in the atmosphere of substellar objects. Understanding the
microphysical and dynamical properties of clouds at these transitions
thus probably remains our best way forward.
}},
doi = {10.3847/2041-8213/aaaa61},
adsurl = {https://ui.adsabs.harvard.edu/abs/2018ApJ...853L..30L},
localpdf = {https://ui.adsabs.harvard.edu/abs/2018ApJ...853L..30L.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}