pubtide0.bib

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@comment{{Command line: bib2bib -c 'not journal:"Discussions"' -c 'not title:"Correction to"' -c 'abstract:"tide" or abstract:"tidal"' -c $type="ARTICLE" -oc pubtide0.txt -ob pubtide0.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},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2019ApJ...875...46Y.pdf},
  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},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2019A_26A...624A..17A.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..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{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{2016A&A...596A.112T,
  author = {{Turbet}, M. and {Leconte}, J. and {Selsis}, F. and {Bolmont}, E. and 
	{Forget}, F. and {Ribas}, I. and {Raymond}, S.~N. and {Anglada-Escudé}, G.
	},
  title = {{The habitability of Proxima Centauri b. II. Possible climates and observability}},
  journal = {\aap},
  archiveprefix = {arXiv},
  eprint = {1608.06827},
  primaryclass = {astro-ph.EP},
  keywords = {stars: individual: Proxima Cen, planets and satellites: individual: Proxima Cen b, planets and satellites: atmospheres, planets and satellites: terrestrial planets, planets and satellites: detection, astrobiology},
  year = 2016,
  volume = 596,
  eid = {A112},
  pages = {A112},
  abstract = {{Radial velocity monitoring has found the signature of a Msini =
1.3M$_{⊕}$ planet located within the habitable zone (HZ) of
Proxima Centauri. Despite a hotter past and an active host star, the
planet Proxima b could have retained enough volatiles to sustain surface
habitability. Here we use a 3D Global Climate Model (GCM) to simulate
the atmosphere and water cycle of Proxima b for its two likely rotation
modes (1:1 and 3:2 spin-orbit resonances), while varying the
unconstrained surface water inventory and atmospheric greenhouse effect.
Any low-obliquity, low-eccentricity planet within the HZ of its star
should be in one of the climate regimes discussed here. We find that a
broad range of atmospheric compositions allow surface liquid water. On a
tidally locked planet with sufficient surface water inventory, liquid
water is always present, at least in the substellar region. With a
non-synchronous rotation, this requires a minimum greenhouse warming (
10 mbar of CO$_{2}$ and 1 bar of N$_{2}$). If the planet is
dryer,  0.5 bar or 1.5 bars of CO$_{2}$ (for asynchronous or
synchronous rotation, respectively) suffice to prevent the trapping of
any arbitrary, small water inventory into polar or nightside ice caps.
We produce reflection and emission spectra and phase curves for the
simulated climates. We find that atmospheric characterization will be
possible via direct imaging with forthcoming large telescopes. The
angular separation of 7{$\lambda$}/D at 1 {$\mu$}m (with the E-ELT) and a
contrast of  10$^{-7}$ will enable high-resolution spectroscopy
and the search for molecular signatures, including H$_{2}$O,
O$_{2}$, and CO$_{2}$. The observation of thermal phase
curves can be attempted with the James Webb Space Telescope, thanks to a
contrast of 2 {\times} 10$^{-5}$ at 10 {$\mu$}m. Proxima b will also
be an exceptional target for future IR interferometers. Within a decade
it will be possible to image Proxima b and possibly determine whether
the surface of this exoplanet is habitable.
}},
  doi = {10.1051/0004-6361/201629577},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2016A%26A...596A.112T},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2016A_26A...596A.112T.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2016Icar..277..196F,
  author = {{Fouchet}, T. and {Greathouse}, T.~K. and {Spiga}, A. and {Fletcher}, L.~N. and 
	{Guerlet}, S. and {Leconte}, J. and {Orton}, G.~S.},
  title = {{Stratospheric aftermath of the 2010 Storm on Saturn as observed by the TEXES instrument. I. Temperature structure}},
  journal = {\icarus},
  archiveprefix = {arXiv},
  eprint = {1604.06479},
  primaryclass = {astro-ph.EP},
  keywords = {Saturn, atmosphere, Atmospheres, structure, Atmospheres, dynamics, Infrared observations},
  year = 2016,
  volume = 277,
  pages = {196-214},
  abstract = {{We report on spectroscopic observations of Saturn's stratosphere in July
2011 with the Texas Echelon Cross Echelle Spectrograph (TEXES) mounted
on the NASA InfraRed Telescope Facility (IRTF). The observations,
targeting several lines of the CH$_{4}${$\nu$}$_{4}$ band and
the H$_{2}$ S(1) quadrupolar line, were designed to determine how
Saturn's stratospheric thermal structure was disturbed by the 2010 Great
White Spot. A study of Cassini Composite Infrared Spectrometer (CIRS)
spectra had already shown the presence of a large stratospheric
disturbance centered at a pressure of 2 hPa, nicknamed the beacon B0,
and a tail of warm air at lower pressures (Fletcher et al. [2012] Icarus
221, 560-586). Our observations confirm that the beacon B0 vertical
structure determined by CIRS, with a maximum temperature of 180 {\plusmn}
1 K at 2 hPa, is overlain by a temperature decrease up to the 0.2-hPa
pressure level. Our retrieved maximum temperature of 180 {\plusmn} 1 K is
colder than that derived by CIRS (200 {\plusmn} 1 K), a difference that
may be quantitatively explained by terrestrial atmospheric smearing. We
propose a scenario for the formation of the beacon based on the
saturation of gravity waves emitted by the GWS. Our observations also
reveal that the tail is a planet-encircling disturbance in Saturn's
upper stratosphere, oscillating between 0.2 and 0.02 hPa, showing a
distinct wavenumber-2 pattern. We propose that this pattern in the upper
stratosphere is either the signature of thermal tides generated by the
presence of the warm beacon in the mid-stratosphere, or the signature of
Rossby wave activity.
}},
  doi = {10.1016/j.icarus.2016.04.030},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2016Icar..277..196F},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2016Icar..277..196F.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2016A&A...591A.106B,
  author = {{Bolmont}, E. and {Libert}, A.-S. and {Leconte}, J. and {Selsis}, F.
	},
  title = {{Habitability of planets on eccentric orbits: Limits of the mean flux approximation}},
  journal = {\aap},
  archiveprefix = {arXiv},
  eprint = {1604.06091},
  primaryclass = {astro-ph.EP},
  keywords = {planets and satellites: atmospheres, planets and satellites: terrestrial planets, methods: numerical},
  year = 2016,
  volume = 591,
  eid = {A106},
  pages = {A106},
  abstract = {{Unlike the Earth, which has a small orbital eccentricity, some
exoplanets discovered in the insolation habitable zone (HZ) have high
orbital eccentricities (e.g., up to an eccentricity of \~{}0.97 for HD
20782 b). This raises the question of whether these planets have surface
conditions favorable to liquid water. In order to assess the
habitability of an eccentric planet, the mean flux approximation is
often used. It states that a planet on an eccentric orbit is called
habitable if it receives on average a flux compatible with the presence
of surface liquid water. However, because the planets experience
important insolation variations over one orbit and even spend some time
outside the HZ for high eccentricities, the question of their
habitability might not be as straightforward. We performed a set of
simulations using the global climate model LMDZ to explore the limits of
the mean flux approximation when varying the luminosity of the host star
and the eccentricity of the planet. We computed the climate of tidally
locked ocean covered planets with orbital eccentricity from 0 to 0.9
receiving a mean flux equal to Earth's. These planets are found around
stars of luminosity ranging from 1 L$_{&sun;}$ to
10$^{-4}$L$_{&sun;}$. We use a definition of habitability
based on the presence of surface liquid water, and find that most of the
planets considered can sustain surface liquid water on the dayside with
an ice cap on the nightside. However, for high eccentricity and high
luminosity, planets cannot sustain surface liquid water during the whole
orbital period. They completely freeze at apoastron and when approaching
periastron an ocean appears around the substellar point. We conclude
that the higher the eccentricity and the higher the luminosity of the
star, the less reliable the mean flux approximation.
}},
  doi = {10.1051/0004-6361/201628073},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2016A%26A...591A.106B},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2016A_26A...591A.106B.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},
  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},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2014RSPTA.37230084F,
  author = {{Forget}, F. and {Leconte}, J.},
  title = {{Possible climates on terrestrial exoplanets}},
  journal = {Philosophical Transactions of the Royal Society of London Series A},
  archiveprefix = {arXiv},
  eprint = {1311.3101},
  primaryclass = {astro-ph.EP},
  year = 2014,
  volume = 372,
  pages = {20130084-20130084},
  abstract = {{What kind of environment may exist on terrestrial planets around other
stars? In spite of the lack of direct observations, it may not be
premature to speculate on exoplanetary climates, for instance to
optimize future telescopic observations, or to assess the probability of
habitable worlds. To first order, climate primarily depends on 1) The
atmospheric composition and the volatile inventory; 2) The incident
stellar flux; 3) The tidal evolution of the planetary spin, which can
notably lock a planet with a permanent night side. The atmospheric
composition and mass depends on complex processes which are difficult to
model: origins of volatile, atmospheric escape, geochemistry,
photochemistry. We discuss physical constraints which can help us to
speculate on the possible type of atmosphere, depending on the planet
size, its final distance for its star and the star type. Assuming that
the atmosphere is known, the possible climates can be explored using
Global Climate Models analogous to the ones developed to simulate the
Earth as well as the other telluric atmospheres in the solar system. Our
experience with Mars, Titan and Venus suggests that realistic climate
simulators can be developed by combining components like a ``dynamical
core'', a radiative transfer solver, a parametrisation of subgrid-scale
turbulence and convection, a thermal ground model, and a volatile phase
change code. On this basis, we can aspire to build reliable climate
predictors for exoplanets. However, whatever the accuracy of the models,
predicting the actual climate regime on a specific planet will remain
challenging because climate systems are affected by strong positive
destabilizing feedbacks (such as runaway glaciations and runaway
greenhouse effect). They can drive planets with very similar forcing and
volatile inventory to completely different states.
}},
  doi = {10.1098/rsta.2013.0084},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2014RSPTA.37230084F},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2014RSPTA.37230084F.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2014A&A...563A.103S,
  author = {{Samuel}, B. and {Leconte}, J. and {Rouan}, D. and {Forget}, F. and 
	{Léger}, A. and {Schneider}, J.},
  title = {{Constraining physics of very hot super-Earths with the James Webb Telescope. The case of CoRot-7b}},
  journal = {\aap},
  archiveprefix = {arXiv},
  eprint = {1402.6637},
  primaryclass = {astro-ph.EP},
  keywords = {planets and satellites: atmospheres, planet-star interactions, planets and satellites: physical evolution, planets and satellites: fundamental parameters, planets and satellites: composition, planets and satellites: surfaces},
  year = 2014,
  volume = 563,
  eid = {A103},
  pages = {A103},
  abstract = {{Context. Transit detection from space using ultra-precise photometry led
to the first detection of super-Earths with solid surfaces: CoRot-7b and
Kepler-10b. Because they lie only a few stellar radii from their host
stars, these two rocky planets are expected to be extremely hot. 

Aims: Assuming that these planets are in a synchronous rotation state
and receive strong stellar winds and fluxes, previous studies have
suggested that they must be atmosphere-free and that a lava ocean is
present on their hot dayside. In this article, we use several dedicated
thermal models of the irradiated planet to study how observations with
NIRSPEC on the James Webb Space Telescope (JWST) could further confirm
and constrain, or reject the atmosphere-free lava ocean planet model for
very hot super-Earths. 
 Methods: Using CoRoT-7b as a working case,
we explore the consequences on the phase-curve of a non tidal-locked
rotation, with the presence/absence of an atmosphere, and for different
values of the surface albedo. We then simulate future observations of
the reflected light and thermal emission from CoRoT-7b with NIRSPEC-JWST
and look for detectable signatures, such as time lag, of those
peculiarities. We also study the possibility to retrieve the latitudinal
surface temperature distribution from the observed SED. 
 Results:
We demonstrate that we should be able to constrain several parameters
after observations of two orbits (42 h) thanks to the broad range of
wavelengths accessible with JWST: i) the Bond albedo is retrieved to
within {\plusmn}0.03 in most cases. ii) The lag effect allows us to
retrieve the rotation period within 3 h of a non phase-locked planet,
whose rotation would be half the orbital period; for longer period, the
accuracy is reduced. iii) Any spin period shorter than a limit in the
range 30-800 h, depending on the thickness of the thermal layer in the
soil, would be detected. iv) The presence of a thick gray atmosphere
with a pressure of one bar, and a specific opacity higher than
10$^{-5}$ m$^{-2}$ kg$^{-1}$ is detectable. v) With
spectra up to 4.5 {$\mu$}m, the latitudinal temperature profile can be
retrieved to within 30 K with a risk of a totally wrong solution in 5\%
of the cases. This last result is obtained for a signal-to-noise ratio
around 5 per resel, which should be reached on Corot-7 after a total
exposure time of \~{}70 h with NIRSPEC and only three hours on a V = 8
star. 
 Conclusions: We conclude that it should thus be possible to
distinguish the reference situation of a lava ocean with phase-locking
and no atmosphere from other cases. In addition, obtaining the surface
temperature map and the albedo brings important constraints on the
nature or the physical state of the soil of hot super-Earths.
}},
  doi = {10.1051/0004-6361/201321039},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2014A%26A...563A.103S},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2014A_26A...563A.103S.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2013Icar..226.1642C,
  author = {{Cébron}, D. and {Le Bars}, M. and {Le Gal}, P. and {Moutou}, C. and 
	{Leconte}, J. and {Sauret}, A.},
  title = {{Elliptical instability in hot Jupiter systems}},
  journal = {\icarus},
  archiveprefix = {arXiv},
  eprint = {1309.1624},
  primaryclass = {astro-ph.SR},
  year = 2013,
  volume = 226,
  pages = {1642-1653},
  abstract = {{Several studies have already considered the influence of tides on the
evolution of systems composed of a star and a close-in companion to
tentatively explain different observations such as the spin-up of some
stars with hot Jupiters, the radius anomaly of short orbital period
planets and the synchronization or quasi-synchronization of the stellar
spin in some extreme cases. However, the nature of the mechanism
responsible for the tidal dissipation in such systems remains uncertain.
In this paper, we claim that the so-called elliptical instability may
play a major role in these systems, explaining some systematic features
present in the observations. This hydrodynamic instability, arising in
rotating flows with elliptical streamlines, is suspected to be present
in both planet and star of such systems, which are elliptically deformed
by tides. The presence and the influence of the elliptical instability
in gaseous bodies, such as stars or hot Jupiters, are most of the time
neglected. In this paper, using numerical simulations and theoretical
arguments, we consider several features associated to the elliptical
instability in hot-Jupiter systems. In particular, the use of ad hoc
boundary conditions makes it possible to estimate the amplitude of the
elliptical instability in gaseous bodies. We also consider the influence
of compressibility on the elliptical instability, and compare the
results to the incompressible case. We demonstrate the ability for the
elliptical instability to grow in the presence of differential rotation,
with a possible synchronized latitude, provided that the tidal
deformation and/or the rotation rate of the fluid are large enough.
Moreover, the amplitude of the instability for a centrally-condensed
mass of fluid is of the same order of magnitude as for an incompressible
fluid for a given distance to the threshold of the instability. Finally,
we show that the assumption of the elliptical instability being the main
tidal dissipation process in eccentric inflated hot Jupiters and
misaligned stars is consistent with current data.
}},
  doi = {10.1016/j.icarus.2012.12.017},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2013Icar..226.1642C},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2013Icar..226.1642C.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2013A&A...556A..17B,
  author = {{Bolmont}, E. and {Selsis}, F. and {Raymond}, S.~N. and {Leconte}, J. and 
	{Hersant}, F. and {Maurin}, A.-S. and {Pericaud}, J.},
  title = {{Tidal dissipation and eccentricity pumping: Implications for the depth of the secondary eclipse of 55 Cancri e}},
  journal = {\aap},
  archiveprefix = {arXiv},
  eprint = {1304.0459},
  primaryclass = {astro-ph.EP},
  keywords = {planets and satellites: fundamental parameters, planets and satellites: dynamical evolution and stability, planet-star interactions},
  year = 2013,
  volume = 556,
  eid = {A17},
  pages = {A17},
  abstract = {{
 Aims: We use the super Earth 55 Cnc e as a case study to address
an observable effect of tidal heating. This transiting short-period
planet belongs to a compact multiple system with massive planets. We
investigate whether planet-planet interactions can force the
eccentricity of this planet to a level affecting the eclipse depth
observed with Spitzer. 
 Methods: Using the constant time lag tidal
model, we first calculate the observed planet flux as a function of
albedo and eccentricity, for different tidal dissipation constants and
for two extreme cases: a planet with no heat redistribution and a planet
with full heat redistribution. We derive the values of albedo and
eccentricity that match the observed transit depth. We then perform
N-body simulations of the planetary system including tides and general
relativity to follow the evolution of the eccentricity of planet e. We
compare the range of eccentricities given by the simulations with the
eccentricities required to alter the eclipse depth. 
 Results:
Using our nominal value for the dissipation constant and the most recent
estimates of the orbital elements and masses of the 55 Cnc planets, we
find that the eccentricity of planet e can be large enough to contribute
at a measurable level to the thermal emission measured with Spitzer.
This affects the constraints on the albedo of the planet, which can be
as high as 0.9 (instead of 0.55 when ignoring tidal heating). We also
derive a maximum value for the eccentricity of planet e directly from
the eclipse depth: e $\lt$ 0.015 assuming Earth's dissipation constant.

 Conclusions: Transiting exoplanets in multiple planet systems -
like 55 Cancri - are exceptional targets for testing tidal models
because their tidal luminosity may be observable. Future
multi-wavelengths observations of eclipse depth and phase curves (for
instance with EChO and JWST) should allow us to better resolve the
temperature map of these planets and break the degeneracy between albedo
and tidal heating that remains for single band observations. In
addition, an accurate determination of the eccentricity will make it
possible to constrain the dissipation rate of the planet and to probe
its internal structure.
}},
  doi = {10.1051/0004-6361/201220837},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2013A%26A...556A..17B},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2013A_26A...556A..17B.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2013A&A...555A..51S,
  author = {{Selsis}, F. and {Maurin}, A.-S. and {Hersant}, F. and {Leconte}, J. and 
	{Bolmont}, E. and {Raymond}, S.~N. and {Delbo'}, M.},
  title = {{The effect of rotation and tidal heating on the thermal lightcurves of super Mercuries}},
  journal = {\aap},
  archiveprefix = {arXiv},
  eprint = {1305.3858},
  primaryclass = {astro-ph.EP},
  keywords = {techniques: photometric, planetary systems},
  year = 2013,
  volume = 555,
  eid = {A51},
  pages = {A51},
  abstract = {{Short-period ($\lt$50 day), low-mass ($\lt$ 10 M$_{⊕}$)
exoplanets are abundant, and the few of them whose radius and mass have
been measured already reveal a diversity in composition. Some of these
exoplanets are found on eccentric orbits and are subjected to strong
tides that affect their rotation and result in significant tidal
heating. Within this population, some planets are likely to be depleted
in volatiles and have no atmosphere. We modeled the thermal emission of
these super Mercuries to study the signatures of rotation and tidal
dissipation on their infrared lightcurve. We computed the time-dependent
temperature map on the surface and in the subsurface of the planet and
the resulting disk-integrated emission spectrum received by a distant
observer for any observation geometry. We calculated the illumination of
the planetary surface for any Keplerian orbit and rotation. We included
the internal tidal heat flow, vertical heat diffusion in the subsurface
and generated synthetic lightcurves. We show that the different rotation
periods predicted by tidal models (spin-orbit resonances,
pseudo-synchronization) produce different photometric signatures, which
are observable provided that the thermal inertia of the surface is high,
as for solid or melted rocks (but not regolith). Tidal dissipation can
also directly affect the lightcurves and make the inference of the
rotation more difficult or easier depending on the existence of hot
spots on the surface. Infrared lightcurve measurement with the James
Webb Space Telescope and EChO can be used to infer exoplanets' rotation
periods and dissipation rates and thus to test tidal models. This data
will also constrain the nature of the (sub)surface by constraining the
thermal inertia.
}},
  doi = {10.1051/0004-6361/201321661},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2013A%26A...555A..51S},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2013A_26A...555A..51S.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2012A&A...544A.124B,
  author = {{Bolmont}, E. and {Raymond}, S.~N. and {Leconte}, J. and {Matt}, S.~P.
	},
  title = {{Effect of the stellar spin history on the tidal evolution of close-in planets}},
  journal = {\aap},
  archiveprefix = {arXiv},
  eprint = {1207.2127},
  primaryclass = {astro-ph.EP},
  keywords = {stars: rotation, planets and satellites: dynamical evolution and stability, planet-star interactions},
  year = 2012,
  volume = 544,
  eid = {A124},
  pages = {A124},
  abstract = {{Context. The spin rate of stars evolves substantially during their
lifetime, owing to the evolution of their internal structure and to
external torques arising from the interaction of stars with their
environments and stellar winds. 
 Aims: We investigate how the
evolution of the stellar spin rate affects, and is affected by, planets
in close orbits via star-planet tidal interactions. 
 Methods: We
used a standard equilibrium tidal model to compute the orbital evolution
of single planets orbiting both Sun-like stars and very low-mass stars
(0.1 M$_{&sun;}$). We tested two stellar spin evolution profiles,
one with fast initial rotation (1.2 day rotation period) and one with
slow initial rotation (8 day period). We tested the effect of varying
the stellar and planetary dissipations, and the planet's mass and
initial orbital radius. 
 Results: For Sun-like stars, the
different tidal evolution between initially rapidly and slowly rotating
stars is only evident for extremely close-in gas giants orbiting highly
dissipative stars. However, for very low-mass stars the effect of the
initial rotation of the star on the planet's evolution is apparent for
less massive (1 M$_{⊕}$) planets and typical dissipation
values. We also find that planetary evolution can have significant
effects on the stellar spin history. In particular, when a planet falls
onto the star, it can cause the star to spin up. 
 Conclusions:
Tidal evolution allows us to differentiate between the early behaviors
of extremely close-in planets orbiting either a rapidly rotating star or
a slowly rotating star. The early spin-up of the star allows the
close-in planets around fast rotators to survive the early evolution.
For planets around M-dwarfs, surviving the early evolution means
surviving on Gyr timescales, whereas for Sun-like stars the spin-down
brings about late mergers of Jupiter planets. In the light of this
study, we can say that differentiating one type of spin evolution from
another given the present position of planets can be very tricky. Unless
we can observe some markers of former evolution, it is nearly impossible
to distinguish the two very different spin profiles, let alone
intermediate spin-profiles. Nevertheless, some conclusions can still be
drawn about statistical distributions of planets around fully convective
M-dwarfs. If tidal evolution brings about a merger late in the stellar
history, it can also entail a noticeable acceleration of the star at
late ages, so that it is possible to have old stars that spin rapidly.
This raises the question of how the age of stars can be more tightly
constrained.
}},
  doi = {10.1051/0004-6361/201219645},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2012A%26A...544A.124B},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2012A_26A...544A.124B.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2011OLEB...41..539H,
  author = {{Heller}, R. and {Barnes}, R. and {Leconte}, J.},
  title = {{Habitability of Extrasolar Planets and Tidal Spin Evolution}},
  journal = {Origins of Life and Evolution of the Biosphere},
  archiveprefix = {arXiv},
  eprint = {1108.4347},
  primaryclass = {astro-ph.EP},
  keywords = {Habitability, Orbital dynamics, Tidal processes, Habitable zone, Gl581d},
  year = 2011,
  volume = 41,
  pages = {539-543},
  abstract = {{Stellar radiation has conservatively been used as the key constraint to
planetary habitability. We review here the effects of tides, exerted by
the host star on the planet, on the evolution of the planetary spin.
Tides initially drive the rotation period and the orientation of the
rotation axis into an equilibrium state but do not necessarily lead to
synchronous rotation. As tides also circularize the orbit, eventually
the rotation period does equal the orbital period and one hemisphere
will be permanently irradiated by the star. Furthermore, the rotational
axis will become perpendicular to the orbit, i.e. the planetary surface
will not experience seasonal variations of the insolation. We illustrate
here how tides alter the spins of planets in the traditional habitable
zone. As an example, we show that, neglecting perturbations due to other
companions, the Super-Earth Gl581d performs two rotations per orbit and
that any primordial obliquity has been eroded.
}},
  doi = {10.1007/s11084-011-9252-3},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2011OLEB...41..539H},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011OLEB...41..539H.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2011A&A...535A..94B,
  author = {{Bolmont}, E. and {Raymond}, S.~N. and {Leconte}, J.},
  title = {{Tidal evolution of planets around brown dwarfs}},
  journal = {\aap},
  archiveprefix = {arXiv},
  eprint = {1109.2906},
  primaryclass = {astro-ph.EP},
  keywords = {brown dwarfs, stars: rotation, planets and satellites: dynamical evolution and stability, planet-star interactions, astrobiology},
  year = 2011,
  volume = 535,
  eid = {A94},
  pages = {A94},
  abstract = {{Context. The tidal evolution of planets orbiting brown dwarfs (BDs)
presents an interesting case study because BDs' terrestrial planet
forming region is located extremely close-in. In fact, the habitable
zones of BDs range from roughly 0.001 to 0.03 AU and for the lowest-mass
BDs are located interior to the Roche limit. 
 Aims: In contrast
with stars, BDs spin up as they age. Thus, the corotation distance moves
inward. This has important implications for the tidal evolution of
planets around BDs. 
 Methods: We used a standard equilibrium tidal
model to compute the orbital evolution of a large ensemble of planet-BD
systems. We tested the effect of numerous parameters such as the initial
semi-major axis and eccentricity, the rotation period of the BD, the
masses of both the BD and planet, and the tidal dissipation factors. 
 Results: We find that all planets that form at or beyond the
corotation distance and with initial eccentricities smaller than \~{}0.1
are repelled from the BD. Some planets initially interior to corotation
can survive if their inward tidal evolution is slower than the BD's spin
evolution, but most initially close-in planets fall onto the BD. 

Conclusions: We find that the most important parameter for the tidal
evolution is the initial orbital distance with respect to the corotation
distance. Some planets can survive in the habitable zone for Gyr
timescales, although in many cases the habitable zone moves inward past
the planet's orbit in just tens to hundreds of Myr. Surviving planets
can have orbital periods of less than 10 days (as small as 10 h), so
they could be observable by transit.
}},
  doi = {10.1051/0004-6361/201117734},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2011A%26A...535A..94B},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...535A..94B.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2011A&A...528A..41L,
  author = {{Leconte}, J. and {Lai}, D. and {Chabrier}, G.},
  title = {{Distorted, nonspherical transiting planets: impact on the transit depth and on the radius determination}},
  journal = {\aap},
  archiveprefix = {arXiv},
  eprint = {1101.2813},
  primaryclass = {astro-ph.EP},
  keywords = {planets and satellites: general, planets and satellites: interiors, planets and satellites: fundamental parameters, equation of state},
  year = 2011,
  volume = 528,
  eid = {A41},
  pages = {A41},
  abstract = {{In this paper, we quantify the systematic impact of the nonspherical
shape of transiting planets caused by tidal forces and rotation on the
observed transit depth. Such a departure from sphericity leads to a bias
in the derivation of the transit radius from the light curve and affects
the comparison with planet structure and evolution models, which assume
spherical symmetry. As the tidally deformed planet projects its smallest
cross section area during the transit, the measured effective radius is
smaller than the one of the unperturbed spherical planet (which is the
radius predicted by 1D evolution models). This effect can be corrected
by calculating the theoretical shape of the observed planet. Using a
variational method and a simple polytropic assumption for the gaseous
planet structure, we derived simple analytical expressions for the
ellipsoidal shape of a fluid object (star or planet) accounting for both
tidal and rotational deformations. We determined the characteristic
polytropic indexes that describe the structures of irradiated close-in
planets within the mass range 0.3 M$_{J}$ $\lt$ M$_{p}$ $\lt$
75 M$_{J}$, at different ages, by comparing polytropic models with
the inner density profiles calculated with the full evolution code. Our
calculations yield a 20\% effect on the transit depth, i.e. a 10\%
decrease in the measured radius, for the extreme case of a 1
M$_{J}$ planet orbiting a Sun-like star at 0.01 AU, and the effect
can be greater for lower mass objects. For the closest planets detected
so far ( {\lsim} 0.05 AU), the effect on the radius is of the order of 1
to 10\%, by no means a negligible effect, enhancing the puzzling problem
of the anomalously large bloated planets. These corrections must thus be
taken into account for correctly determining the radius from the transit
light curve and when comparing theoretical models with observations. Our
analytical expressions can be easily used to calculate these
corrections, caused by the nonspherical shape of the planet, on the
observed transit depth and thus to derive the planet's real equilibrium
radius, the one to be used when comparing models with observations. They
can also be used to model ellipsoidal variations in the stellar flux now
detected in the CoRoT and Kepler light curves. We also derive directly
usable analytical expressions for the moment of inertia and the Love
number (k$_{2}$) of a fluid planet as a function of its mass and,
in the case of significant rotation, for its oblateness.

Tables B.2 and B.3 are only available in electronic form at http://www.aanda.org
}},
  doi = {10.1051/0004-6361/201015811},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2011A%26A...528A..41L},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..41L.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2011A&A...528A..27H,
  author = {{Heller}, R. and {Leconte}, J. and {Barnes}, R.},
  title = {{Tidal obliquity evolution of potentially habitable planets}},
  journal = {\aap},
  archiveprefix = {arXiv},
  eprint = {1101.2156},
  primaryclass = {astro-ph.EP},
  keywords = {planets and satellites: dynamical evolution and stability, celestial mechanics, planet-star interactions, astrobiology, stars: low-mass, planets and satellites: tectonics},
  year = 2011,
  volume = 528,
  eid = {A27},
  pages = {A27},
  abstract = {{Context. Stellar insolation has been used as the main constraint on a
planet's potential habitability. However, as more Earth-like planets are
discovered around low-mass stars (LMSs), a re-examination of the role of
tides on the habitability of exoplanets has begun. Those studies have
yet to consider the misalignment between a planet's rotational axis and
the orbital plane normal, i.e. the planetary obliquity. 
 Aims:
This paper considers the constraints on habitability arising from tidal
processes due to the planet's spin orientation and rate. Since tidal
processes are far from being understood we seek to understand
differences between commonly used tidal models. 
 Methods: We apply
two equilibrium tide theories - a constant-phase-lag model and a
constant-time-lag model - to compute the obliquity evolution of
terrestrial planets orbiting in the habitable zones around LMSs. The
time for the obliquity to decrease from an Earth-like obliquity of
23.5{\deg} to 5{\deg}, the ``tilt erosion time'', is compared to the
traditional insolation habitable zone (IHZ) in the parameter space
spanned by the semi-major axis a, the eccentricity e, and the stellar
mass M$_{s}$. We also compute tidal heating and equilibrium
rotation caused by obliquity tides as further constraints on
habitability. The Super-Earth Gl581 d and the planet candidate Gl581 g
are studied as examples for these tidal processes. 
 Results:
Earth-like obliquities of terrestrial planets in the IHZ around stars
with masses {\lsim} 0.25 M$_{&sun;}$ are eroded in less than 0.1
Gyr. Only terrestrial planets orbiting stars with masses {\gsim} 0.9
M$_{&sun;}$ experience tilt erosion times larger than 1 Gyr
throughout the IHZ. Tilt erosion times for terrestrial planets in highly
eccentric orbits inside the IHZ of solar-like stars can be {\lsim} 10
Gyr. Terrestrial planets in the IHZ of stars with masses {\lsim} 0.25
M$_{&sun;}$ undergo significant tidal heating due to obliquity
tides, whereas in the IHZ of stars with masses {\gsim} 0.5
M$_{&sun;}$ they require additional sources of heat to drive
tectonic activity. The predictions of the two tidal models diverge
significantly for e {\gsim} 0.3. In our two-body simulations, Gl581 d's
obliquity is eroded to 0{\deg} and its rotation period reached its
equilibrium state of half its orbital period in $\lt$ 0.1 Gyr. Tidal
surface heating on the putative Gl581 g is {\lsim} 150 mW/m$^{2}$
as long as its eccentricity is smaller than 0.3. 
 Conclusions:
Obliquity tides modify the concept of the habitable zone. Tilt erosion
of terrestrial planets orbiting LMSs should be included by atmospheric
modelers. Tidal heating needs to be considered by geologists.
}},
  doi = {10.1051/0004-6361/201015809},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2011A%26A...528A..27H},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2011A_26A...528A..27H.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2010A&A...516A..64L,
  author = {{Leconte}, J. and {Chabrier}, G. and {Baraffe}, I. and {Levrard}, B.
	},
  title = {{Is tidal heating sufficient to explain bloated exoplanets? Consistent calculations accounting for finite initial eccentricity}},
  journal = {\aap},
  archiveprefix = {arXiv},
  eprint = {1004.0463},
  primaryclass = {astro-ph.EP},
  keywords = {brown dwarfs, planet-star interactions, planets and satellites: dynamical evolution and stability, planets and satellites: general},
  year = 2010,
  volume = 516,
  eid = {A64},
  pages = {A64},
  abstract = {{We present the consistent evolution of short-period exoplanets coupling
the tidal and gravothermal evolution of the planet. Contrarily to
previous similar studies, our calculations are based on the complete
tidal evolution equations of the Hut (1981) model, valid at any order in
eccentricity, obliquity and spin. We demonstrate both analytically and
numerically that except if the system was formed with a nearly circular
orbit (e {\lap} 0.2), consistently solving the complete tidal equations
is mandatory to derive correct tidal evolution histories. We show that
calculations based on tidal models truncated at 2nd order in
eccentricity, as done in all previous studies, lead to quantitatively
and sometimes even qualitatively erroneous tidal evolutions. As a
consequence, tidal energy dissipation rates are severely underestimated
in all these calculations and the characteristic timescales for the
various orbital parameters evolutions can be wrong by up to three orders
of magnitude. These discrepancies can by no means be justified by
invoking the uncertainty in the tidal quality factors. Based on these
complete, consistent calculations, we revisit the viability of the tidal
heating hypothesis to explain the anomalously large radius of transiting
giant planets. We show that even though tidal dissipation does provide a
substantial contribution to the planet's heat budget and can explain
some of the moderately bloated hot-Jupiters, this mechanism can not
explain alone the properties of the most inflated objects, including HD
209 458 b. Indeed, solving the complete tidal equations shows that
enhanced tidal dissipation and thus orbit circularization occur too
early during the planet's evolution to provide enough extra energy at
the present epoch. In that case either a third, so far undetected,
low-mass companion must be present to keep exciting the eccentricity of
the giant planet, or other mechanisms - stellar irradiation induced
surface winds dissipating in the planet's tidal bulges and thus reaching
the convective layers, inefficient flux transport by convection in the
planet's interior - must be invoked, together with tidal dissipation, to
provide all the pieces of the abnormally large exoplanet puzzle.
}},
  doi = {10.1051/0004-6361/201014337},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2010A%26A...516A..64L},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2010A_26A...516A..64L.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2009A&A...506..385L,
  author = {{Leconte}, J. and {Baraffe}, I. and {Chabrier}, G. and {Barman}, T. and 
	{Levrard}, B.},
  title = {{Structure and evolution of the first CoRoT exoplanets: probing the brown dwarf/planet overlapping mass regime}},
  journal = {\aap},
  archiveprefix = {arXiv},
  eprint = {0907.2669},
  primaryclass = {astro-ph.EP},
  keywords = {stars: low-mass, brown dwarfs, stars: planetary systems},
  year = 2009,
  volume = 506,
  pages = {385-389},
  abstract = {{We present detailed structure and evolution calculations for the first
transiting extrasolar planets discovered by the space-based CoRoT
mission. Comparisons between theoretical and observed radii provide
information on the internal composition of the CoRoT objects. We
distinguish three different categories of planets emerging from these
discoveries and from previous ground-based surveys: (i) planets
explained by standard planetary models including irradiation; (ii)
abnormally bloated planets; and (iii) massive objects belonging to the
overlapping mass regime between planets and brown dwarfs. For the second
category, we show that tidal heating can explain the relevant CoRoT
objects, providing non-zero eccentricities. We stress that the usual
assumption of a quick circularization of the orbit by tides, as usually
done in transit light curve analysis, is not justified a priori, as
suggested recently by Levrard et al. (2009), and that eccentricity
analysis should be carefully redone for some observations. Finally,
special attention is devoted to CoRoT-3b and to the identification of
its very nature: giant planet or brown dwarf? The radius determination
of this object confirms the theoretical mass-radius predictions for
gaseous bodies in the substellar regime but, given the present
observational uncertainties, does not allow an unambiguous
identification of its very nature. This opens the avenue, however, to an
observational identification of these two distinct astrophysical
populations, brown dwarfs and giant planets, in their overlapping mass
range, as done for the case of the 8 Jupiter-mass object Hat-P-2b.
According to the presently published error bars for the radius
determination and to our present theoretical description of planet
structure and evolution, the high mean density of this object requires a
substantial metal enrichment of the interior and is inconsistent at
about the 2-sigma limit with the expected radius of a solar-metallicity
brown dwarf. Within the aforementioned observational and theoretical
determinations, this allows a clear identification of its planetary
nature, suggesting that planets may form up to at least 8 Jupiter
masses.
}},
  doi = {10.1051/0004-6361/200911896},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2009A%26A...506..385L},
  localpdf = {https://ui.adsabs.harvard.edu/abs/2009A_26A...506..385L.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}