pub2013.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=2013 -c $type="ARTICLE" -oc pub2013.txt -ob pub2013.bib leconte.link.bib}}
@article{2013Natur.504..268L,
author = {{Leconte}, J. and {Forget}, F. and {Charnay}, B. and {Wordsworth}, R. and
{Pottier}, A.},
title = {{Increased insolation threshold for runaway greenhouse processes on Earth-like planets}},
journal = {\nat},
archiveprefix = {arXiv},
eprint = {1312.3337},
primaryclass = {astro-ph.EP},
year = 2013,
volume = 504,
pages = {268-271},
abstract = {{The increase in solar luminosity over geological timescales should warm
the Earth's climate, increasing water evaporation, which will in turn
enhance the atmospheric greenhouse effect. Above a certain critical
insolation, this destabilizing greenhouse feedback can `run away' until
the oceans have completely evaporated. Through increases in
stratospheric humidity, warming may also cause evaporative loss of the
oceans to space before the runaway greenhouse state occurs. The critical
insolation thresholds for these processes, however, remain uncertain
because they have so far been evaluated using one-dimensional models
that cannot account for the dynamical and cloud feedback effects that
are key stabilizing features of the Earth's climate. Here we use a
three-dimensional global climate model to show that the insolation
threshold for the runaway greenhouse state to occur is about 375 W
m$^{-2}$, which is significantly higher than previously thought.
Our model is specifically developed to quantify the climate response of
Earth-like planets to increased insolation in hot and extremely moist
atmospheres. In contrast with previous studies, we find that clouds have
a destabilizing feedback effect on the long-term warming. However,
subsident, unsaturated regions created by the Hadley circulation have a
stabilizing effect that is strong enough to shift the runaway greenhouse
limit to higher values of insolation than are inferred from
one-dimensional models. Furthermore, because of wavelength-dependent
radiative effects, the stratosphere remains sufficiently cold and dry to
hamper the escape of atmospheric water, even at large fluxes. This has
strong implications for the possibility of liquid water existing on
Venus early in its history, and extends the size of the habitable zone
around other stars.
}},
doi = {10.1038/nature12827},
adsurl = {https://ui.adsabs.harvard.edu/abs/2013Natur.504..268L},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013Natur.504..268L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013Natur.504..268L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013Natur.504..268L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013Natur.504..268L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013Natur.504..268L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013Natur.504..268L.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},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013Icar..226.1642C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013Icar..226.1642C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013Icar..226.1642C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013Icar..226.1642C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013Icar..226.1642C.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2013JGRD..11810414C,
author = {{Charnay}, B. and {Forget}, F. and {Wordsworth}, R. and {Leconte}, J. and
{Millour}, E. and {Codron}, F. and {Spiga}, A.},
title = {{Exploring the faint young Sun problem and the possible climates of the Archean Earth with a 3-D GCM}},
journal = {Journal of Geophysical Research (Atmospheres)},
archiveprefix = {arXiv},
eprint = {1310.4286},
primaryclass = {astro-ph.EP},
keywords = {early Earth, Archean, paleo-climates},
year = 2013,
volume = 118,
number = d17,
pages = {10},
abstract = {{Different solutions have been proposed to solve the ``faint young Sun
problem,'' defined by the fact that the Earth was not fully frozen during
the Archean despite the fainter Sun. Most previous studies were
performed with simple 1-D radiative convective models and did not
account well for the clouds and ice-albedo feedback or the atmospheric
and oceanic transport of energy. We apply a global climate model (GCM)
to test the different solutions to the faint young Sun problem. We
explore the effect of greenhouse gases (CO$_{2}$ and
CH$_{4}$), atmospheric pressure, cloud droplet size, land
distribution, and Earth's rotation rate. We show that neglecting organic
haze, 100 mbar of CO$_{2}$ with 2 mbar of CH$_{4}$ at 3.8 Ga
and 10 mbar of CO$_{2}$ with 2 mbar of CH$_{4}$ at 2.5 Ga
allow a temperate climate (mean surface temperature between 10{\deg}C and
20{\deg}C). Such amounts of greenhouse gases remain consistent with the
geological data. Removing continents produces a warming lower than
+4{\deg}C. The effect of rotation rate is even more limited. Larger
droplets (radii of 17 {$\mu$}m versus 12 {$\mu$}m) and a doubling of the
atmospheric pressure produce a similar warming of around +7{\deg}C. In
our model, ice-free water belts can be maintained up to 25{\deg}N/S with
less than 1 mbar of CO$_{2}$ and no methane. An interesting cloud
feedback appears above cold oceans, stopping the glaciation. Such a
resistance against full glaciation tends to strongly mitigate the faint
young Sun problem.
}},
doi = {10.1002/jgrd.50808},
adsurl = {https://ui.adsabs.harvard.edu/abs/2013JGRD..11810414C},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013JGRD..11810414C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013JGRD..11810414C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013JGRD..11810414C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013JGRD..11810414C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013JGRD..11810414C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013JGRD..11810414C.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},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013A_26A...556A..17B.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013A_26A...556A..17B.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013A_26A...556A..17B.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013A_26A...556A..17B.pdf},
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},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013A_26A...555A..51S.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013A_26A...555A..51S.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013A_26A...555A..51S.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013A_26A...555A..51S.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013A_26A...555A..51S.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2013A&A...554A..69L,
author = {{Leconte}, J. and {Forget}, F. and {Charnay}, B. and {Wordsworth}, R. and
{Selsis}, F. and {Millour}, E. and {Spiga}, A.},
title = {{3D climate modeling of close-in land planets: Circulation patterns, climate moist bistability, and habitability}},
journal = {\aap},
archiveprefix = {arXiv},
eprint = {1303.7079},
primaryclass = {astro-ph.EP},
keywords = {planets and satellites: general, planets and satellites: atmospheres, planets and satellites: physical evolution, planet-star interactions},
year = 2013,
volume = 554,
eid = {A69},
pages = {A69},
abstract = {{The inner edge of the classical habitable zone is often defined by the
critical flux needed to trigger the runaway greenhouse instability. This
1D notion of a critical flux, however, may not be all that relevant for
inhomogeneously irradiated planets, or when the water content is limited
(land planets). Based on results from our 3D global climate model, we
present general features of the climate and large-scale circulation on
close-in terrestrial planets. We find that the circulation pattern can
shift from super-rotation to stellar/anti stellar circulation when the
equatorial Rossby deformation radius significantly exceeds the planetary
radius, changing the redistribution properties of the atmosphere. Using
analytical and numerical arguments, we also demonstrate the presence of
systematic biases among mean surface temperatures and among temperature
profiles predicted from either 1D or 3D simulations. After including a
complete modeling of the water cycle, we further demonstrate that two
stable climate regimes can exist for land planets closer than the inner
edge of the classical habitable zone. One is the classical runaway state
where all the water is vaporized, and the other is a collapsed state
where water is captured in permanent cold traps. We identify this
``moist'' bistability as the result of a competition between the
greenhouse effect of water vapor and its condensation on the night side
or near the poles, highlighting the dynamical nature of the runaway
greenhouse effect. We also present synthetic spectra showing the
observable signature of these two states. Taking the example of two
prototype planets in this regime, namely Gl 581 c and HD 85512 b, we
argue that depending on the rate of water delivery and atmospheric
escape during the life of these planets, they could accumulate a
significant amount of water ice at their surface. If such a thick ice
cap is present, various physical mechanisms observed on Earth (e.g.,
gravity driven ice flows, geothermal flux) should come into play to
produce long-lived liquid water at the edge and/or bottom of the ice
cap. Consequently, the habitability of planets at smaller orbital
distance than the inner edge of the classical habitable zone cannot be
ruled out. Transiting planets in this regime represent promising targets
for upcoming exoplanet characterization observatories, such as EChO and
JWST.
}},
doi = {10.1051/0004-6361/201321042},
adsurl = {https://ui.adsabs.harvard.edu/abs/2013A%26A...554A..69L},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013A_26A...554A..69L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013A_26A...554A..69L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013A_26A...554A..69L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013A_26A...554A..69L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013A_26A...554A..69L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013A_26A...554A..69L.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2013NatGe...6..347L,
author = {{Leconte}, J. and {Chabrier}, G.},
title = {{Layered convection as the origin of Saturn's luminosity anomaly}},
journal = {Nature Geoscience},
archiveprefix = {arXiv},
eprint = {1304.6184},
primaryclass = {astro-ph.EP},
year = 2013,
volume = 6,
pages = {347-350},
abstract = {{As the giant planets of our Solar System continue to cool and contract,
they radiate more energy than they receive from the Sun. A giant
planet's cooling rate, luminosity and temperature at a given age can be
determined using the first and second principles of thermodynamics.
Measurements of Saturn's infrared luminosity, however, reveal that
Saturn is significantly brighter than predicted for its age. This excess
luminosity has been attributed to the immiscibility of helium in
Saturn's hydrogen-rich envelope, which leads to rains of helium-rich
droplets. Existing calculations of Saturn's evolution, however, suggest
that the energy released by helium rains might be insufficient to
resolve the luminosity puzzle. Here we demonstrate, using
semi-analytical models of planetary thermal evolution, that the cooling
of Saturn's interior is significantly slower in the presence of layered
convection generated--like in Earth's oceans--by a compositional
gradient. We find that layered convection can explain Saturn's present
luminosity for a wide range of initial energy configurations without
invoking any additional energy source. Our findings suggest that the
interior structure, composition and thermal evolution of giant planets
in our Solar System and beyond may be more complex than the conventional
approximation of giant planets as homogeneous adiabatic bodies.
}},
doi = {10.1038/ngeo1791},
adsurl = {https://ui.adsabs.harvard.edu/abs/2013NatGe...6..347L},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013NatGe...6..347L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013NatGe...6..347L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013NatGe...6..347L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013NatGe...6..347L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013NatGe...6..347L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013NatGe...6..347L.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2013Icar..222...81F,
author = {{Forget}, F. and {Wordsworth}, R. and {Millour}, E. and {Madeleine}, J.-B. and
{Kerber}, L. and {Leconte}, J. and {Marcq}, E. and {Haberle}, R.~M.
},
title = {{3D modelling of the early martian climate under a denser CO$_{2}$ atmosphere: Temperatures and CO$_{2}$ ice clouds}},
journal = {\icarus},
archiveprefix = {arXiv},
eprint = {1210.4216},
primaryclass = {astro-ph.EP},
year = 2013,
volume = 222,
pages = {81-99},
abstract = {{On the basis of geological evidence, it is often stated that the early
martian climate was warm enough for liquid water to flow on the surface
thanks to the greenhouse effect of a thick atmosphere. We present 3D
global climate simulations of the early martian climate performed
assuming a faint young Sun and a CO$_{2}$ atmosphere with surface
pressure between 0.1 and 7 bars. The model includes a detailed radiative
transfer model using revised CO$_{2}$ gas collision induced
absorption properties, and a parameterisation of the CO$_{2}$ ice
cloud microphysical and radiative properties. A wide range of possible
climates is explored using various values of obliquities, orbital
parameters, cloud microphysic parameters, atmospheric dust loading, and
surface properties. Unlike on present day Mars, for pressures higher
than a fraction of a bar, surface temperatures vary with altitude
because of the adiabatic cooling and warming of the atmosphere when it
moves vertically. In most simulations, CO$_{2}$ ice clouds cover a
major part of the planet. Previous studies had suggested that they could
have warmed the planet thanks to their scattering greenhouse effect.
However, even assuming parameters that maximize this effect, it does not
exceed +15 K. Combined with the revised CO$_{2}$ spectroscopy and
the impact of surface CO$_{2}$ ice on the planetary albedo, we
find that a CO$_{2}$ atmosphere could not have raised the annual
mean temperature above 0 {\deg}C anywhere on the planet. The collapse of
the atmosphere into permanent CO$_{2}$ ice caps is predicted for
pressures higher than 3 bar, or conversely at pressure lower than 1 bar
if the obliquity is low enough. Summertime diurnal mean surface
temperatures above 0 {\deg}C (a condition which could have allowed rivers
and lakes to form) are predicted for obliquity larger than 40{\deg} at
high latitudes but not in locations where most valley networks or
layered sedimentary units are observed. In the absence of other warming
mechanisms, our climate model results are thus consistent with a cold
early Mars scenario in which nonclimatic mechanisms must occur to
explain the evidence for liquid water. In a companion paper by
Wordsworth et al. we simulate the hydrological cycle on such a planet
and discuss how this could have happened in more detail.
}},
doi = {10.1016/j.icarus.2012.10.019},
adsurl = {https://ui.adsabs.harvard.edu/abs/2013Icar..222...81F},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013Icar..222...81F.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013Icar..222...81F.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013Icar..222...81F.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013Icar..222...81F.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013Icar..222...81F.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2013Icar..222...81F.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}