pub2015.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=2015 -c $type="ARTICLE" -oc pub2015.txt -ob pub2015.bib leconte.link.bib}}
@article{2015ExA....40..449L,
author = {{Leconte}, J. and {Forget}, F. and {Lammer}, H.},
title = {{On the (anticipated) diversity of terrestrial planet atmospheres}},
journal = {Experimental Astronomy},
keywords = {Planet, Atmosphere, Composition, Climate regime},
year = 2015,
volume = 40,
pages = {449-467},
abstract = {{On our way toward the characterization of smaller and more temperate
planets, missions dedicated to the spectroscopic observation of
exoplanets will teach us about the wide diversity of classes of
planetary atmospheres, many of them probably having no equivalent in the
Solar System. But what kind of atmospheres can we expect? To start
answering this question, many theoretical studies have tried to
understand and model the various processes controlling the formation and
evolution of planetary atmospheres, with some success in the Solar
System. Here, we shortly review these processes and we try to give an
idea of the various type of atmospheres that these processes can create.
As will be made clear, current atmosphere evolution models have many
shortcomings yet, and need heavy calibrations. With that in mind, we
will thus discuss how observations with a mission similar to EChO would
help us unravel the link between a planet's environment and its
atmosphere.
}},
doi = {10.1007/s10686-014-9403-4},
adsurl = {https://ui.adsabs.harvard.edu/abs/2015ExA....40..449L},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015ExA....40..449L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015ExA....40..449L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015ExA....40..449L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015ExA....40..449L.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2015ExA....40..329T,
author = {{Tinetti}, G. and {Drossart}, P. and {Eccleston}, P. and {Hartogh}, P. and
{Isaak}, K. and {Linder}, M. and {Lovis}, C. and {Micela}, G. and
{Ollivier}, M. and {Puig}, L. and {Ribas}, I. and {Snellen}, I. and
{Swinyard}, B. and {Allard}, F. and {Barstow}, J. and {Cho}, J. and
{Coustenis}, A. and {Cockell}, C. and {Correia}, A. and {Decin}, L. and
{de Kok}, R. and {Deroo}, P. and {Encrenaz}, T. and {Forget}, F. and
{Glasse}, A. and {Griffith}, C. and {Guillot}, T. and {Koskinen}, T. and
{Lammer}, H. and {Leconte}, J. and {Maxted}, P. and {Mueller-Wodarg}, I. and
{Nelson}, R. and {North}, C. and {Pallé}, E. and {Pagano}, I. and
{Piccioni}, G. and {Pinfield}, D. and {Selsis}, F. and {Sozzetti}, A. and
{Stixrude}, L. and {Tennyson}, J. and {Turrini}, D. and {Zapatero-Osorio}, M. and
{Beaulieu}, J.-P. and {Grodent}, D. and {Guedel}, M. and {Luz}, D. and
{N{\o}rgaard-Nielsen}, H.~U. and {Ray}, T. and {Rickman}, H. and
{Selig}, A. and {Swain}, M. and {Banaszkiewicz}, M. and {Barlow}, M. and
{Bowles}, N. and {Branduardi-Raymont}, G. and {du Foresto}, V.~C. and
{Gerard}, J.-C. and {Gizon}, L. and {Hornstrup}, A. and {Jarchow}, C. and
{Kerschbaum}, F. and {Kovacs}, G. and {Lagage}, P.-O. and {Lim}, T. and
{Lopez-Morales}, M. and {Malaguti}, G. and {Pace}, E. and {Pascale}, E. and
{Vandenbussche}, B. and {Wright}, G. and {Ramos Zapata}, G. and
{Adriani}, A. and {Azzollini}, R. and {Balado}, A. and {Bryson}, I. and
{Burston}, R. and {Colomé}, J. and {Crook}, M. and {Di Giorgio}, A. and
{Griffin}, M. and {Hoogeveen}, R. and {Ottensamer}, R. and {Irshad}, R. and
{Middleton}, K. and {Morgante}, G. and {Pinsard}, F. and {Rataj}, M. and
{Reess}, J.-M. and {Savini}, G. and {Schrader}, J.-R. and {Stamper}, R. and
{Winter}, B. and {Abe}, L. and {Abreu}, M. and {Achilleos}, N. and
{Ade}, P. and {Adybekian}, V. and {Affer}, L. and {Agnor}, C. and
{Agundez}, M. and {Alard}, C. and {Alcala}, J. and {Allende Prieto}, C. and
{Alonso Floriano}, F.~J. and {Altieri}, F. and {Alvarez Iglesias}, C.~A. and
{Amado}, P. and {Andersen}, A. and {Aylward}, A. and {Baffa}, C. and
{Bakos}, G. and {Ballerini}, P. and {Banaszkiewicz}, M. and
{Barber}, R.~J. and {Barrado}, D. and {Barton}, E.~J. and {Batista}, V. and
{Bellucci}, G. and {Belmonte Avilés}, J.~A. and {Berry}, D. and
{Bézard}, B. and {Biondi}, D. and {B{\l}{\c e}cka}, M. and
{Boisse}, I. and {Bonfond}, B. and {Bordé}, P. and {B{\"o}rner}, P. and
{Bouy}, H. and {Brown}, L. and {Buchhave}, L. and {Budaj}, J. and
{Bulgarelli}, A. and {Burleigh}, M. and {Cabral}, A. and {Capria}, M.~T. and
{Cassan}, A. and {Cavarroc}, C. and {Cecchi-Pestellini}, C. and
{Cerulli}, R. and {Chadney}, J. and {Chamberlain}, S. and {Charnoz}, S. and
{Christian Jessen}, N. and {Ciaravella}, A. and {Claret}, A. and
{Claudi}, R. and {Coates}, A. and {Cole}, R. and {Collura}, A. and
{Cordier}, D. and {Covino}, E. and {Danielski}, C. and {Damasso}, M. and
{Deeg}, H.~J. and {Delgado-Mena}, E. and {Del Vecchio}, C. and
{Demangeon}, O. and {De Sio}, A. and {De Wit}, J. and {Dobrijévic}, M. and
{Doel}, P. and {Dominic}, C. and {Dorfi}, E. and {Eales}, S. and
{Eiroa}, C. and {Espinoza Contreras}, M. and {Esposito}, M. and
{Eymet}, V. and {Fabrizio}, N. and {Fern{\'a}ndez}, M. and {Femen{\'{\i}}a Castella}, B. and
{Figueira}, P. and {Filacchione}, G. and {Fletcher}, L. and
{Focardi}, M. and {Fossey}, S. and {Fouqué}, P. and {Frith}, J. and
{Galand}, M. and {Gambicorti}, L. and {Gaulme}, P. and {Garc{\'{\i}}a L{\'o}pez}, R.~J. and
{Garcia-Piquer}, A. and {Gear}, W. and {Gerard}, J.-C. and {Gesa}, L. and
{Giani}, E. and {Gianotti}, F. and {Gillon}, M. and {Giro}, E. and
{Giuranna}, M. and {Gomez}, H. and {Gomez-Leal}, I. and {Gonzalez Hernandez}, J. and
{Gonz{\'a}lez Merino}, B. and {Graczyk}, R. and {Grassi}, D. and
{Guardia}, J. and {Guio}, P. and {Gustin}, J. and {Hargrave}, P. and
{Haigh}, J. and {Hébrard}, E. and {Heiter}, U. and {Heredero}, R.~L. and
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{Hubert}, B. and {Hueso}, R. and {Israelian}, G. and {Iro}, N. and
{Irwin}, P. and {Jacquemoud}, S. and {Jones}, G. and {Jones}, H. and
{Justtanont}, K. and {Kehoe}, T. and {Kerschbaum}, F. and {Kerins}, E. and
{Kervella}, P. and {Kipping}, D. and {Koskinen}, T. and {Krupp}, N. and
{Lahav}, O. and {Laken}, B. and {Lanza}, N. and {Lellouch}, E. and
{Leto}, G. and {Licandro Goldaracena}, J. and {Lithgow-Bertelloni}, C. and
{Liu}, S.~J. and {Lo Cicero}, U. and {Lodieu}, N. and {Lognonné}, P. and
{Lopez-Puertas}, M. and {Lopez-Valverde}, M.~A. and {Lundgaard Rasmussen}, I. and
{Luntzer}, A. and {Machado}, P. and {MacTavish}, C. and {Maggio}, A. and
{Maillard}, J.-P. and {Magnes}, W. and {Maldonado}, J. and {Mall}, U. and
{Marquette}, J.-B. and {Mauskopf}, P. and {Massi}, F. and {Maurin}, A.-S. and
{Medvedev}, A. and {Michaut}, C. and {Miles-Paez}, P. and {Montalto}, M. and
{Monta{\~n}és Rodr{\'{\i}}guez}, P. and {Monteiro}, M. and
{Montes}, D. and {Morais}, H. and {Morales}, J.~C. and {Morales-Calder{\'o}n}, M. and
{Morello}, G. and {Moro Mart{\'{\i}}n}, A. and {Moses}, J. and
{Moya Bedon}, A. and {Murgas Alcaino}, F. and {Oliva}, E. and
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{Parmentier}, V. and {Parviainen}, H. and {Pe{\~n}a Ram{\'{\i}}rez}, K.~Y. and
{Peralta}, J. and {Perez-Hoyos}, S. and {Petrov}, R. and {Pezzuto}, S. and
{Pietrzak}, R. and {Pilat-Lohinger}, E. and {Piskunov}, N. and
{Prinja}, R. and {Prisinzano}, L. and {Polichtchouk}, I. and
{Poretti}, E. and {Radioti}, A. and {Ramos}, A.~A. and {Rank-L{\"u}ftinger}, T. and
{Read}, P. and {Readorn}, K. and {Rebolo L{\'o}pez}, R. and
{Rebord{\~a}o}, J. and {Rengel}, M. and {Rezac}, L. and {Rocchetto}, M. and
{Rodler}, F. and {S{\'a}nchez Béjar}, V.~J. and {Sanchez Lavega}, A. and
{Sanrom{\'a}}, E. and {Santos}, N. and {Sanz Forcada}, J. and
{Scandariato}, G. and {Schmider}, F.-X. and {Scholz}, A. and
{Scuderi}, S. and {Sethenadh}, J. and {Shore}, S. and {Showman}, A. and
{Sicardy}, B. and {Sitek}, P. and {Smith}, A. and {Soret}, L. and
{Sousa}, S. and {Stiepen}, A. and {Stolarski}, M. and {Strazzulla}, G. and
{Tabernero}, H.~M. and {Tanga}, P. and {Tecsa}, M. and {Temple}, J. and
{Terenzi}, L. and {Tessenyi}, M. and {Testi}, L. and {Thompson}, S. and
{Thrastarson}, H. and {Tingley}, B.~W. and {Trifoglio}, M. and
{Mart{\'{\i}}n Torres}, J. and {Tozzi}, A. and {Turrini}, D. and
{Varley}, R. and {Vakili}, F. and {de Val-Borro}, M. and {Valdivieso}, M.~L. and
{Venot}, O. and {Villaver}, E. and {Vinatier}, S. and {Viti}, S. and
{Waldmann}, I. and {Waltham}, D. and {Ward-Thompson}, D. and
{Waters}, R. and {Watkins}, C. and {Watson}, D. and {Wawer}, P. and
{Wawrzaszk}, A. and {White}, G. and {Widemann}, T. and {Winek}, W. and
{Wi{\'s}niowski}, T. and {Yelle}, R. and {Yung}, Y. and {Yurchenko}, S.~N.
},
title = {{The EChO science case}},
journal = {Experimental Astronomy},
archiveprefix = {arXiv},
eprint = {1502.05747},
primaryclass = {astro-ph.EP},
keywords = {Exoplanets, Spectroscopy, Atmospheric science, IR astronomy, Space missions},
year = 2015,
volume = 40,
pages = {329-391},
abstract = {{The discovery of almost two thousand exoplanets has revealed an
unexpectedly diverse planet population. We see gas giants in few-day
orbits, whole multi-planet systems within the orbit of Mercury, and new
populations of planets with masses between that of the Earth and
Neptune{\mdash}all unknown in the Solar System. Observations to date have
shown that our Solar System is certainly not representative of the
general population of planets in our Milky Way. The key science
questions that urgently need addressing are therefore: What are
exoplanets made of? Why are planets as they are? How do planetary
systems work and what causes the exceptional diversity observed as
compared to the Solar System? The EChO (Exoplanet Characterisation
Observatory) space mission was conceived to take up the challenge to
explain this diversity in terms of formation, evolution, internal
structure and planet and atmospheric composition. This requires in-depth
spectroscopic knowledge of the atmospheres of a large and well-defined
planet sample for which precise physical, chemical and dynamical
information can be obtained. In order to fulfil this ambitious
scientific program, EChO was designed as a dedicated survey mission for
transit and eclipse spectroscopy capable of observing a large, diverse
and well-defined planet sample within its 4-year mission lifetime. The
transit and eclipse spectroscopy method, whereby the signal from the
star and planet are differentiated using knowledge of the planetary
ephemerides, allows us to measure atmospheric signals from the planet at
levels of at least 10$^{-4}$ relative to the star. This can only
be achieved in conjunction with a carefully designed stable payload and
satellite platform. It is also necessary to provide broad instantaneous
wavelength coverage to detect as many molecular species as possible, to
probe the thermal structure of the planetary atmospheres and to correct
for the contaminating effects of the stellar photosphere. This requires
wavelength coverage of at least 0.55 to 11 {$\mu$}m with a goal of covering
from 0.4 to 16 {$\mu$}m. Only modest spectral resolving power is needed,
with R \~{} 300 for wavelengths less than 5 {$\mu$}m and R \~{} 30 for
wavelengths greater than this. The transit spectroscopy technique means
that no spatial resolution is required. A telescope collecting area of
about 1 m$^{2}$ is sufficiently large to achieve the necessary
spectro-photometric precision: for the Phase A study a 1.13
m$^{2}$ telescope, diffraction limited at 3 {$\mu$}m has been
adopted. Placing the satellite at L2 provides a cold and stable thermal
environment as well as a large field of regard to allow efficient
time-critical observation of targets randomly distributed over the sky.
EChO has been conceived to achieve a single goal: exoplanet
spectroscopy. The spectral coverage and signal-to-noise to be achieved
by EChO, thanks to its high stability and dedicated design, would be a
game changer by allowing atmospheric composition to be measured with
unparalleled exactness: at least a factor 10 more precise and a factor
10 to 1000 more accurate than current observations. This would enable
the detection of molecular abundances three orders of magnitude lower
than currently possible and a fourfold increase from the handful of
molecules detected to date. Combining these data with estimates of
planetary bulk compositions from accurate measurements of their radii
and masses would allow degeneracies associated with planetary interior
modelling to be broken, giving unique insight into the interior
structure and elemental abundances of these alien worlds. EChO would
allow scientists to study exoplanets both as a population and as
individuals. The mission can target super-Earths, Neptune-like, and
Jupiter-like planets, in the very hot to temperate zones (planet
temperatures of 300-3000 K) of F to M-type host stars. The EChO core
science would be delivered by a three-tier survey. The EChO Chemical
Census: This is a broad survey of a few-hundred exoplanets, which allows
us to explore the spectroscopic and chemical diversity of the exoplanet
population as a whole. The EChO Origin: This is a deep survey of a
subsample of tens of exoplanets for which significantly higher signal to
noise and spectral resolution spectra can be obtained to explain the
origin of the exoplanet diversity (such as formation mechanisms,
chemical processes, atmospheric escape). The EChO Rosetta Stones: This
is an ultra-high accuracy survey targeting a subsample of select
exoplanets. These will be the bright ``benchmark'' cases for which a large
number of measurements would be taken to explore temporal variations,
and to obtain two and three dimensional spatial information on the
atmospheric conditions through eclipse-mapping techniques. If EChO were
launched today, the exoplanets currently observed are sufficient to
provide a large and diverse sample. The Chemical Census survey would
consist of $\gt$ 160 exoplanets with a range of planetary sizes,
temperatures, orbital parameters and stellar host properties.
Additionally, over the next 10 years, several new ground- and
space-based transit photometric surveys and missions will come on-line
(e.g. NGTS, CHEOPS, TESS, PLATO), which will specifically focus on
finding bright, nearby systems. The current rapid rate of discovery
would allow the target list to be further optimised in the years prior
to EChO's launch and enable the atmospheric characterisation of hundreds
of planets.
}},
doi = {10.1007/s10686-015-9484-8},
adsurl = {https://ui.adsabs.harvard.edu/abs/2015ExA....40..329T},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015ExA....40..329T.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015ExA....40..329T.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015ExA....40..329T.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015ExA....40..329T.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2015ApJ...813L...1C,
author = {{Charnay}, B. and {Meadows}, V. and {Misra}, A. and {Leconte}, J. and
{Arney}, G.},
title = {{3D Modeling of GJ1214b{\rsquo}s Atmosphere: Formation of Inhomogeneous High Clouds and Observational Implications}},
journal = {\apjl},
archiveprefix = {arXiv},
eprint = {1510.01706},
primaryclass = {astro-ph.EP},
keywords = {planets and satellites: atmospheres, planets and satellites: individual: GJ1214b},
year = 2015,
volume = 813,
eid = {L1},
pages = {L1},
abstract = {{The warm sub-Neptune GJ1214b has a featureless transit spectrum that may
be due to the presence of high and thick clouds or haze. Here, we
simulate the atmosphere of GJ1214b with a 3D General Circulation Model
for cloudy hydrogen-dominated atmospheres, including cloud radiative
effects. We show that the atmospheric circulation is strong enough to
transport micrometric cloud particles to the upper atmosphere and
generally leads to a minimum of cloud at the equator. By scattering
stellar light, clouds increase the planetary albedo to 0.4-0.6 and
cool the atmosphere below 1 mbar. However, the heating by ZnS clouds
leads to the formation of a stratospheric thermal inversion above 10
mbar, with temperatures potentially high enough on the dayside to
evaporate KCl clouds. We show that flat transit spectra consistent with
Hubble Space Telescope observations are possible if cloud particle radii
are around 0.5 {$\mu$}m, and that such clouds should be optically thin at
wavelengths $\gt$3 {$\mu$}m. Using simulated cloudy atmospheres that fit the
observed spectra we generate transit, emission, and reflection spectra
and phase curves for GJ1214b. We show that a stratospheric thermal
inversion would be readily accessible in near- and mid-infrared
atmospheric spectral windows. We find that the amplitude of the thermal
phase curves is strongly dependent on metallicity, but only slightly
impacted by clouds. Our results suggest that primary and secondary
eclipses and phase curves observed by the James Webb Space Telescope in
the near- to mid-infrared should provide strong constraints on the
nature of GJ1214b's atmosphere and clouds.
}},
doi = {10.1088/2041-8205/813/1/L1},
adsurl = {https://ui.adsabs.harvard.edu/abs/2015ApJ...813L...1C},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015ApJ...813L...1C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015ApJ...813L...1C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015ApJ...813L...1C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015ApJ...813L...1C.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2015ApJ...813...15C,
author = {{Charnay}, B. and {Meadows}, V. and {Leconte}, J.},
title = {{3D Modeling of GJ1214b's Atmosphere: Vertical Mixing Driven by an Anti-Hadley Circulation}},
journal = {\apj},
archiveprefix = {arXiv},
eprint = {1509.06814},
primaryclass = {astro-ph.EP},
keywords = {planets and satellites: atmospheres, planets and satellites: individual: GJ1214b},
year = 2015,
volume = 813,
eid = {15},
pages = {15},
abstract = {{GJ1214b is a warm sub-Neptune transiting in front of a nearby M dwarf
star. Recent observations indicate the presence of high and thick clouds
or haze whose presence requires strong atmospheric mixing. In order to
understand the transport and distribution of such clouds/haze, we study
the atmospheric circulation and the vertical mixing of GJ1214b with a 3D
General Circulation Model for cloud-free hydrogen-dominated atmospheres
(metallicity of 1, 10, and 100 times the solar value) and for a
water-dominated atmosphere. We analyze the effect of the atmospheric
metallicity on the thermal structure and zonal winds. We also analyze
the zonal mean meridional circulation and show that it corresponds to an
anti-Hadley circulation in most of the atmosphere with upwelling at
mid-latitude and downwelling at the equator on average. This circulation
must be present on a large range of synchronously rotating exoplanets
with a strong impact on cloud formation and distribution. Using simple
tracers, we show that vertical winds on GJ1214b can be strong enough to
loft micrometric particles and that the anti-Hadley circulation leads to
a minimum of tracers at the equator. We find that the strength of the
vertical mixing increases with metallicity. We derive 1D equivalent eddy
diffusion coefficients and find simple parametrizations from
$\{$K$\}$$_{{zz}$$\}$=7{\times} $\{$10$\}$$^{2}${\times}
$\{$P$\}$$_{{bar}$$\}$$^{-0.4}$ $\{$$\{$$\{$m$\}$$\}$$\}$$^{2}$
$\{$$\{$$\{$s$\}$$\}$$\}$$^{-1}$ for solar metallicity to
$\{$K$\}$$_{{zz}$$\}$=3{\times} $\{$10$\}$$^{3}${\times}
$\{$P$\}$$_{{bar}$$\}$$^{-0.4}$ $\{$$\{$$\{$m$\}$$\}$$\}$$^{2}$
$\{$$\{$$\{$s$\}$$\}$$\}$$^{-1}$ for the 100{\times} solar metallicity. These values
should favor an efficient formation of photochemical haze in the upper
atmosphere of GJ1214b.
}},
doi = {10.1088/0004-637X/813/1/15},
adsurl = {https://ui.adsabs.harvard.edu/abs/2015ApJ...813...15C},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015ApJ...813...15C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015ApJ...813...15C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015ApJ...813...15C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015ApJ...813...15C.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2015A&A...583A.116B,
author = {{Bolmont}, E. and {Raymond}, S.~N. and {Leconte}, J. and {Hersant}, F. and
{Correia}, A.~C.~M.},
title = {{Mercury-T: A new code to study tidally evolving multi-planet systems. Applications to Kepler-62}},
journal = {\aap},
archiveprefix = {arXiv},
eprint = {1507.04751},
primaryclass = {astro-ph.EP},
keywords = {planets and satellites: dynamical evolution and stability, planets and satellites: terrestrial planets, planets and satellites: individual: Kepler 62, planet-star interactions},
year = 2015,
volume = 583,
eid = {A116},
pages = {A116},
abstract = {{A large proportion of observed planetary systems contain several planets
in a compact orbital configuration, and often harbor at least one
close-in object. These systems are then most likely tidally evolving. We
investigate how the effects of planet-planet interactions influence the
tidal evolution of planets. We introduce for that purpose a new
open-source addition to the MercuryN-body code, Mercury-T, which takes
into account tides, general relativity and the effect of
rotation-induced flattening in order to simulate the dynamical and tidal
evolution of multi-planet systems. It uses a standard equilibrium tidal
model, the constant time lag model. Besides, the evolution of the radius
of several host bodies has been implemented (brown dwarfs, M-dwarfs of
mass 0.1 M$_{&sun;}$, Sun-like stars, Jupiter). We validate the
new code by comparing its output for one-planet systems to the secular
equations results. We find that this code does respect the conservation
of total angular momentum. We applied this new tool to the planetary
system Kepler-62. We find that tides influence the stability of the
system in some cases. We also show that while the four inner planets of
the systems are likely to have slow rotation rates and small
obliquities, the fifth planet could have a fast rotation rate and a high
obliquity. This means that the two habitable zone planets of this
system, Kepler-62e ad f are likely to have very different climate
features, and this of course would influence their potential at hosting
surface liquid water.
The code is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr
(ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/583/A116
}},
doi = {10.1051/0004-6361/201525909},
adsurl = {https://ui.adsabs.harvard.edu/abs/2015A%26A...583A.116B},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015A_26A...583A.116B.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015A_26A...583A.116B.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015A_26A...583A.116B.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015A_26A...583A.116B.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2015Sci...347..632L,
author = {{Leconte}, J. and {Wu}, H. and {Menou}, K. and {Murray}, N.},
title = {{Asynchronous rotation of Earth-mass planets in the habitable zone of lower-mass stars}},
journal = {Science},
archiveprefix = {arXiv},
eprint = {1502.01952},
primaryclass = {astro-ph.EP},
year = 2015,
volume = 347,
pages = {632-635},
abstract = {{Planets in the habitable zone of lower-mass stars are often assumed to
be in a state of tidally synchronized rotation, which would considerably
affect their putative habitability. Although thermal tides cause Venus
to rotate retrogradely, simple scaling arguments tend to attribute this
peculiarity to the massive Venusian atmosphere. Using a global climate
model, we show that even a relatively thin atmosphere can drive
terrestrial planets{\rsquo} rotation away from synchronicity. We derive a
more realistic atmospheric tide model that predicts four asynchronous
equilibrium spin states, two being stable, when the amplitude of the
thermal tide exceeds a threshold that is met for habitable Earth-like
planets with a 1-bar atmosphere around stars more massive than \~{}0.5 to
0.7 solar mass. Thus, many recently discovered terrestrial planets could
exhibit asynchronous spin-orbit rotation, even with a thin atmosphere.
}},
doi = {10.1126/science.1258686},
adsurl = {https://ui.adsabs.harvard.edu/abs/2015Sci...347..632L},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015Sci...347..632L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015Sci...347..632L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015Sci...347..632L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2015Sci...347..632L.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}