pub2014.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=2014 -c $type="ARTICLE" -oc pub2014.txt -ob pub2014.bib leconte.link.bib}}
@article{2014A&A...572A.109D,
author = {{D{\'{\i}}az}, R.~F. and {Montagnier}, G. and {Leconte}, J. and
{Bonomo}, A.~S. and {Deleuil}, M. and {Almenara}, J.~M. and
{Barros}, S.~C.~C. and {Bouchy}, F. and {Bruno}, G. and {Damiani}, C. and
{Hébrard}, G. and {Moutou}, C. and {Santerne}, A.},
title = {{SOPHIE velocimetry of Kepler transit candidates. XIII. KOI-189 b and KOI-686 b: two very low-mass stars in long-period orbits}},
journal = {\aap},
archiveprefix = {arXiv},
eprint = {1410.5248},
primaryclass = {astro-ph.SR},
keywords = {techniques: photometric, techniques: radial velocities, stars: low-mass, stars: fundamental parameters, stars: individual: KIC11391018, stars: individual: KIC7906882},
year = 2014,
volume = 572,
eid = {A109},
pages = {A109},
abstract = {{We present the radial-velocity follow-up of two Kepler planetary
transiting candidates (KOI-189 and KOI-686) carried out with the SOPHIE
spectrograph at the Observatoire de Haute Provence. These data promptly
discard these objects as viable planet candidates and show that the
transiting objects are in the regime of very low-mass stars, where a
strong discrepancy between observations and models persists for the mass
and radius parameters. By combining the SOPHIE spectra with the Kepler
light curve and photometric measurements found in the literature, we
obtain a full characterization of the transiting companions, their
orbits, and their host stars. The two companions are in significantly
eccentric orbits with relatively long periods (30 days and 52.5 days),
which makes them suitable objects for a comparison with theoretical
models, since the effects invoked to understand the discrepancy with
observations are weaker for these orbital distances. KOI-189 b has a
mass M = 0.0745 {\plusmn} 0.0033 M$_{&sun;}$ and a radius R =
0.1025 {\plusmn} 0.0024 R$_{&sun;}$. The density of KOI-189 b is
significantly lower than expected from theoretical models for a system
of its age. We explore possible explanations for this difference.
KOI-189 b is the smallest hydrogen-burning star with such a precise
determination of its fundamental parameters. KOI-686 b is larger and
more massive (M = 0.0915 {\plusmn} 0.0043 M$_{&sun;}$; R = 0.1201
{\plusmn} 0.0033 R$_{&sun;}$), and its position in the mass-radius
diagram agrees well with theoretical expectations.
Based on observations collected with the SOPHIE spectrograph on the 1.93
m telescope at Observatoire de Haute-Provence (CNRS), France (programs
11A.PNP.MOUT and 11B.PNP.MOUT).Tables 1, 2, and 6 are available in
electronic form at http://www.aanda.org
}},
doi = {10.1051/0004-6361/201424406},
adsurl = {https://ui.adsabs.harvard.edu/abs/2014A%26A...572A.109D},
localpdf = {https://ui.adsabs.harvard.edu/abs/2014A_26A...572A.109D.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2014A_26A...572A.109D.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2014A_26A...572A.109D.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2014A_26A...572A.109D.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2014A_26A...572A.109D.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2014Icar..238..110G,
author = {{Guerlet}, S. and {Spiga}, A. and {Sylvestre}, M. and {Indurain}, M. and
{Fouchet}, T. and {Leconte}, J. and {Millour}, E. and {Wordsworth}, R. and
{Capderou}, M. and {Bézard}, B. and {Forget}, F.},
title = {{Global climate modeling of Saturn{\rsquo}s atmosphere. Part I: Evaluation of the radiative transfer model}},
journal = {\icarus},
year = 2014,
volume = 238,
pages = {110-124},
abstract = {{We have developed and optimized a seasonal, radiative-convective model
of Saturn{\rsquo}s upper troposphere and stratosphere. It is used to
investigate Saturn{\rsquo}s radiatively-forced thermal structure between
3 and 10$^{-6}$ bar, and is intended to be included in a Saturn
global climate model (GCM), currently under development. The main
elements of the radiative transfer model are detailed as well as the
sensitivity to spectroscopic parameters, hydrocarbon abundances, aerosol
properties, oblateness, and ring shadowing effects. The vertical
temperature structure and meridional seasonal contrasts obtained by the
model are then compared to Cassini/CIRS observations. Several
significant model-observation mismatches reveal that Saturn{\rsquo}s
atmosphere departs from radiative equilibrium. For instance, we find
that the modeled temperature profile is close to isothermal above the
2-mbar level, while the temperature retrieved from ground-based or
Cassini/CIRS data continues to increase with altitude. Also, no local
temperature minimum associated to the ring shadowing is observed in the
data, while the model predicts stratospheric temperatures 10 K to 20 K
cooler than in the absence of rings at winter tropical latitudes. These
anomalies are strong evidence that processes other that radiative
heating and cooling control Saturn{\rsquo}s stratospheric thermal
structure. Finally, the model is used to study the warm stratospheric
anomaly triggered after the 2010 Great White Spot. Comparison with
recent Cassini/CIRS observations suggests that the rapid cooling phase
of this warm {\ldquo}beacon{\rdquo} in May-June 2011 can be explained by
radiative processes alone. Observations on a longer timeline are needed
to better characterize and understand its long-term evolution.
}},
doi = {10.1016/j.icarus.2014.05.010},
adsurl = {https://ui.adsabs.harvard.edu/abs/2014Icar..238..110G},
localpdf = {https://ui.adsabs.harvard.edu/abs/2014Icar..238..110G.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2014Icar..238..110G.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2014Icar..238..110G.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2014Icar..238..110G.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2014Icar..238..110G.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},
localpdf = {https://ui.adsabs.harvard.edu/abs/2014RSPTA.37230084F.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2014RSPTA.37230084F.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2014RSPTA.37230084F.pdf},
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},
localpdf = {https://ui.adsabs.harvard.edu/abs/2014A_26A...563A.103S.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2014A_26A...563A.103S.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2014A_26A...563A.103S.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2014A_26A...563A.103S.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}