pub2017.bib
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@article{2017E&PSL.476...11T,
author = {{Turbet}, M. and {Forget}, F. and {Leconte}, J. and {Charnay}, B. and
{Tobie}, G.},
title = {{CO$_{2}$ condensation is a serious limit to the deglaciation of Earth-like planets}},
journal = {Earth and Planetary Science Letters},
archiveprefix = {arXiv},
eprint = {1703.04624},
primaryclass = {astro-ph.EP},
keywords = {climate, snowball, exoplanet, CO$_{2}$ condensation, habitability, climate cycling},
year = 2017,
volume = 476,
pages = {11-21},
abstract = {{It is widely believed that the carbonate-silicate cycle is the main
agent, through volcanism, to trigger deglaciations by CO$_{2}$
greenhouse warming on Earth and on Earth-like planets when they get in a
frozen state. Here we use a 3D Global Climate Model to simulate the
ability of planets initially completely frozen to escape from glaciation
episodes by accumulating enough gaseous CO$_{2}$. The model
includes CO$_{2}$ condensation and sublimation processes and the
water cycle. We find that planets with Earth-like characteristics (size,
mass, obliquity, rotation rate, etc.) orbiting a Sun-like star may never
be able to escape from a glaciation era, if their orbital distance is
greater than {\sim}1.27 Astronomical Units (Flux $\lt$ 847
Wm$^{-2}$ or 62\% of the Solar constant), because CO$_{2}$
would condense at the poles - here the cold traps - forming permanent
CO$_{2}$ ice caps. This limits the amount of CO$_{2}$ in the
atmosphere and thus its greenhouse effect. Furthermore, our results
indicate that for (1) high rotation rates (P$_{rot}$ $\lt$ 24 h),
(2) low obliquity (obliquity $\lt$23.5{\deg}), (3) low background gas
partial pressures ($\lt$1 bar), and (4) high water ice albedo
(H$_{2}$O albedo $\gt$ 0.6), this critical limit could occur at a
significantly lower equivalent distance (or higher insolation). For each
possible configuration, we show that the amount of CO$_{2}$ that
can be trapped in the polar caps depends on the efficiency of
CO$_{2}$ ice to flow laterally as well as its gravitational
stability relative to subsurface water ice. We find that a frozen
Earth-like planet located at 1.30 AU of a Sun-like star could store as
much as 1.5, 4.5 and 15 bars of dry ice at the poles, for internal heat
fluxes of 100, 30 and 10 mW m$^{-2}$, respectively. But these
amounts are in fact lower limits. For planets with a significant water
ice cover, we show that CO$_{2}$ ice deposits should be
gravitationally unstable. They get buried beneath the water ice cover in
geologically short timescales of {\sim}10$^{4}$ yrs, mainly
controlled by the viscosity of water ice. CO$_{2}$ would be
permanently sequestered underneath the water ice cover, in the form of
CO$_{2}$ liquids, CO$_{2}$ clathrate hydrates and/or
dissolved in subglacial water reservoirs (if any). This would
considerably increase the amount of CO$_{2}$ trapped and further
reduce the probability of deglaciation.
}},
doi = {10.1016/j.epsl.2017.07.050},
adsurl = {https://ui.adsabs.harvard.edu/abs/2017E%26PSL.476...11T},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017E_26PSL.476...11T.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017E_26PSL.476...11T.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2017Icar..294..262C,
author = {{Cébron}, D. and {Bars}, M.~L. and {Gal}, P.~L. and {Moutou}, C. and
{Leconte}, J. and {Sauret}, A.},
title = {{Corrigendum to ;Elliptical instability in hot Jupiter systems; ICARUS, Volume 226, Issue 2, November-December 2013, Pages 1642-1653}},
journal = {\icarus},
year = 2017,
volume = 294,
pages = {262-262},
abstract = {{The author regret for the corrections and wishes to replace the below
}},
doi = {10.1016/j.icarus.2017.04.023},
adsurl = {https://ui.adsabs.harvard.edu/abs/2017Icar..294..262C},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017Icar..294..262C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017Icar..294..262C.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2017AJ....154..121B,
author = {{Bourrier}, V. and {de Wit}, J. and {Bolmont}, E. and {Stamenkovi{\'c}}, V. and
{Wheatley}, P.~J. and {Burgasser}, A.~J. and {Delrez}, L. and
{Demory}, B.-O. and {Ehrenreich}, D. and {Gillon}, M. and {Jehin}, E. and
{Leconte}, J. and {Lederer}, S.~M. and {Lewis}, N. and {Triaud}, A.~H.~M.~J. and
{Van Grootel}, V.},
title = {{Temporal Evolution of the High-energy Irradiation and Water Content of TRAPPIST-1 Exoplanets}},
journal = {\aj},
archiveprefix = {arXiv},
eprint = {1708.09484},
primaryclass = {astro-ph.EP},
keywords = {planetary systems, planets and satellites: atmospheres, planets and satellites: terrestrial planets, stars: individual: TRAPPIST-1, stars: low-mass, ultraviolet: planetary systems},
year = 2017,
volume = 154,
eid = {121},
pages = {121},
abstract = {{The ultracool dwarf star TRAPPIST-1 hosts seven Earth-size transiting
planets, some of which could harbor liquid water on their surfaces.
Ultraviolet observations are essential to measuring their high-energy
irradiation and searching for photodissociated water escaping from their
putative atmospheres. Our new observations of the TRAPPIST-1 Ly{$\alpha$}
line during the transit of TRAPPIST-1c show an evolution of the star
an extended hydrogen exosphere. Based on the current knowledge of the
stellar irradiation, we investigated the likely history of water loss in
the system. Planets b to d might still be in a runaway phase, and
planets within the orbit of TRAPPIST-1g could have lost more than 20
Earth oceans after 8 Gyr of hydrodynamic escape. However, TRAPPIST-1e to
h might have lost less than three Earth oceans if hydrodynamic escape
stopped once they entered the habitable zone (HZ). We caution that these
estimates remain limited by the large uncertainty on the planet masses.
They likely represent upper limits on the actual water loss because our
assumptions maximize the X-rays to ultraviolet-driven escape, while
photodissociation in the upper atmospheres should be the limiting
process. Late-stage outgassing could also have contributed significant
amounts of water for the outer, more massive planets after they entered
the HZ. While our results suggest that the outer planets are the best
candidates to search for water with the JWST, they also highlight the
need for theoretical studies and complementary observations in all
wavelength domains to determine the nature of the TRAPPIST-1 planets and
their potential habitability.
}},
doi = {10.3847/1538-3881/aa859c},
adsurl = {https://ui.adsabs.harvard.edu/abs/2017AJ....154..121B},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017AJ....154..121B.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017AJ....154..121B.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2017Icar..291....1C,
author = {{Cavalié}, T. and {Venot}, O. and {Selsis}, F. and {Hersant}, F. and
{Hartogh}, P. and {Leconte}, J.},
title = {{Thermochemistry and vertical mixing in the tropospheres of Uranus and Neptune: How convection inhibition can affect the derivation of deep oxygen abundances}},
journal = {\icarus},
archiveprefix = {arXiv},
eprint = {1703.04358},
primaryclass = {astro-ph.EP},
keywords = {Abundances, Atmospheres, Interior, Uranus, Neptune},
year = 2017,
volume = 291,
pages = {1-16},
abstract = {{Thermochemical models have been used in the past to constrain the deep
oxygen abundance in the gas and ice giant planets from tropospheric CO
spectroscopic measurements. Knowing the oxygen abundance of these
planets is a key to better understand their formation. These models have
widely used dry and/or moist adiabats to extrapolate temperatures from
the measured values in the upper troposphere down to the level where the
thermochemical equilibrium between H$_{2}$O and CO is established.
The mean molecular mass gradient produced by the condensation of
H$_{2}$O stabilizes the atmosphere against convection and results
in a vertical thermal profile and H$_{2}$O distribution that
departs significantly from previous estimates. We revisit O/H estimates
using an atmospheric structure that accounts for the inhibition of the
convection by condensation. We use a thermochemical network and the
latest observations of CO in Uranus and Neptune to calculate the
internal oxygen enrichment required to satisfy both these new estimates
of the thermal profile and the observations. We also present the current
limitations of such modeling.
}},
doi = {10.1016/j.icarus.2017.03.015},
adsurl = {https://ui.adsabs.harvard.edu/abs/2017Icar..291....1C},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017Icar..291....1C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017Icar..291....1C.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2017NatAs...1E.129L,
author = {{Luger}, R. and {Sestovic}, M. and {Kruse}, E. and {Grimm}, S.~L. and
{Demory}, B.-O. and {Agol}, E. and {Bolmont}, E. and {Fabrycky}, D. and
{Fernandes}, C.~S. and {Van Grootel}, V. and {Burgasser}, A. and
{Gillon}, M. and {Ingalls}, J.~G. and {Jehin}, E. and {Raymond}, S.~N. and
{Selsis}, F. and {Triaud}, A.~H.~M.~J. and {Barclay}, T. and
{Barentsen}, G. and {Howell}, S.~B. and {Delrez}, L. and {de Wit}, J. and
{Foreman-Mackey}, D. and {Holdsworth}, D.~L. and {Leconte}, J. and
{Lederer}, S. and {Turbet}, M. and {Almleaky}, Y. and {Benkhaldoun}, Z. and
{Magain}, P. and {Morris}, B.~M. and {Heng}, K. and {Queloz}, D.
},
title = {{A seven-planet resonant chain in TRAPPIST-1}},
journal = {Nature Astronomy},
archiveprefix = {arXiv},
eprint = {1703.04166},
primaryclass = {astro-ph.EP},
year = 2017,
volume = 1,
eid = {0129},
pages = {0129},
abstract = {{The TRAPPIST-1 system is the first transiting planet system found
orbiting an ultracool dwarf star$^{ 1 }$. At least seven planets
similar in radius to Earth were previously found to transit this host
star$^{ 2 }$. Subsequently, TRAPPIST-1 was observed as part of the
K2 mission and, with these new data, we report the measurement of an
18.77 day orbital period for the outermost transiting planet, TRAPPIST-1
h, which was previously unconstrained. This value matches our
theoretical expectations based on Laplace relations$^{ 3 }$ and
places TRAPPIST-1 h as the seventh member of a complex chain, with
three-body resonances linking every member. We find that TRAPPIST-1 h
has a radius of 0.752 R $_{⊕}$ and an equilibrium
temperature of 173{\thinsp}K. We have also measured the rotational period
of the star to be 3.3 days and detected a number of flares consistent
with a low-activity, middle-aged, late M dwarf.
}},
doi = {10.1038/s41550-017-0129},
adsurl = {https://ui.adsabs.harvard.edu/abs/2017NatAs...1E.129L},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017NatAs...1E.129L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017NatAs...1E.129L.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2017Icar..287...54F,
author = {{Forget}, F. and {Bertrand}, T. and {Vangvichith}, M. and {Leconte}, J. and
{Millour}, E. and {Lellouch}, E.},
title = {{A post-new horizons global climate model of Pluto including the N$_{2}$, CH$_{4}$ and CO cycles}},
journal = {\icarus},
keywords = {Pluto, Pluto, atmosphere, Atmospheres, composition, Atmospheres, dynamics},
year = 2017,
volume = 287,
pages = {54-71},
abstract = {{We have built a new 3D Global Climate Model (GCM) to simulate Pluto as
observed by New Horizons in 2015. All key processes are parametrized on
the basis of theoretical equations, including atmospheric dynamics and
transport, turbulence, radiative transfer, molecular conduction, as well
as phases changes for N$_{2}$, CH$_{2}$ and CO. Pluto's
climate and ice cycles are found to be very sensitive to model
parameters and initial states. Nevertheless, a reference simulation is
designed by running a fast, reduced version of the GCM with simplified
atmospheric transport for 40,000 Earth years to initialize the surface
ice distribution and sub-surface temperatures, from which a
28-Earth-year full GCM simulation is performed. Assuming a topographic
depression in a Sputnik-planum (SP)-like crater on the anti-Charon
hemisphere, a realistic Pluto is obtained, with most N$_{2}$ and
CO ices accumulated in the crater, methane frost covering both
hemispheres except for the equatorial regions, and a surface pressure
near 1.1 Pa in 2015 with an increase between 1988 and 2015, as reported
from stellar occultations. Temperature profiles are in qualitative
agreement with the observations. In particular, a cold atmospheric layer
is obtained in the lowest kilometers above Sputnik Planum, as observed
by New Horizons's REX experiment. It is shown to result from the
combined effect of the topographic depression and N$_{2}$ daytime
sublimation. In the reference simulation with surface N$_{2}$ ice
exclusively present in Sputnik Planum, the global circulation is only
forced by radiative heating gradients and remains relatively weak.
Surface winds are locally induced by topography slopes and by
N$_{2}$ condensation and sublimation around Sputnik Planum.
However, the circulation can be more intense depending on the exact
distribution of surface N$_{2}$ frost. This is illustrated in an
alternative simulation with N$_{2}$ condensing in the South Polar
regions and N$_{2}$ frost covering latitudes between 35{\deg}N and
48{\deg}N. A global condensation flow is then created, inducing strong
surface winds everywhere, a prograde jet in the southern high latitudes,
and an equatorial superrotation likely forced by barotropic
instabilities in the southern jet. Using realistic parameters, the GCM
predict atmospheric concentrations of CO and CH$_{4}$ in good
agreement with the observations. N$_{2}$ and CO do not condense in
the atmosphere, but CH$_{4}$ ice clouds can form during daytime at
low altitude near the regions covered by N$_{2}$ ice (assuming
that nucleation is efficient enough). This global climate model can be
used to study many aspects of the Pluto environment. For instance,
organic hazes are included in the GCM and analysed in a companion paper
(Bertrand and Forget, Icarus, this issue).
}},
doi = {10.1016/j.icarus.2016.11.038},
adsurl = {https://ui.adsabs.harvard.edu/abs/2017Icar..287...54F},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017Icar..287...54F.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017Icar..287...54F.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2017Natur.542..456G,
author = {{Gillon}, M. and {Triaud}, A.~H.~M.~J. and {Demory}, B.-O. and
{Jehin}, E. and {Agol}, E. and {Deck}, K.~M. and {Lederer}, S.~M. and
{de Wit}, J. and {Burdanov}, A. and {Ingalls}, J.~G. and {Bolmont}, E. and
{Leconte}, J. and {Raymond}, S.~N. and {Selsis}, F. and {Turbet}, M. and
{Barkaoui}, K. and {Burgasser}, A. and {Burleigh}, M.~R. and
{Carey}, S.~J. and {Chaushev}, A. and {Copperwheat}, C.~M. and
{Delrez}, L. and {Fernandes}, C.~S. and {Holdsworth}, D.~L. and
{Kotze}, E.~J. and {Van Grootel}, V. and {Almleaky}, Y. and
{Benkhaldoun}, Z. and {Magain}, P. and {Queloz}, D.},
title = {{Seven temperate terrestrial planets around the nearby ultracool dwarf star TRAPPIST-1}},
journal = {\nat},
archiveprefix = {arXiv},
eprint = {1703.01424},
primaryclass = {astro-ph.EP},
year = 2017,
volume = 542,
pages = {456-460},
abstract = {{One aim of modern astronomy is to detect temperate, Earth-like
exoplanets that are well suited for atmospheric characterization.
Recently, three Earth-sized planets were detected that transit (that is,
pass in front of) a star with a mass just eight per cent that of the
Sun, located 12 parsecs away. The transiting configuration of these
planets, combined with the Jupiter-like size of their host
star{\mdash}named TRAPPIST-1{\mdash}makes possible in-depth studies of
their atmospheric properties with present-day and future astronomical
facilities. Here we report the results of a photometric monitoring
campaign of that star from the ground and space. Our observations reveal
that at least seven planets with sizes and masses similar to those of
Earth revolve around TRAPPIST-1. The six inner planets form a
near-resonant chain, such that their orbital periods (1.51, 2.42, 4.04,
6.06, 9.1 and 12.35 days) are near-ratios of small integers. This
architecture suggests that the planets formed farther from the star and
migrated inwards. Moreover, the seven planets have equilibrium
temperatures low enough to make possible the presence of liquid water on
their surfaces.
}},
doi = {10.1038/nature21360},
adsurl = {https://ui.adsabs.harvard.edu/abs/2017Natur.542..456G},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017Natur.542..456G.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017Natur.542..456G.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2017A&A...598A..98L,
author = {{Leconte}, J. and {Selsis}, F. and {Hersant}, F. and {Guillot}, T.
},
title = {{Condensation-inhibited convection in hydrogen-rich atmospheres . Stability against double-diffusive processes and thermal profiles for Jupiter, Saturn, Uranus, and Neptune}},
journal = {\aap},
archiveprefix = {arXiv},
eprint = {1610.05506},
primaryclass = {astro-ph.EP},
keywords = {planets and satellites: atmospheres, convection},
year = 2017,
volume = 598,
eid = {A98},
pages = {A98},
abstract = {{In an atmosphere, a cloud condensation region is characterized by a
strong vertical gradient in the abundance of the related condensing
species. On Earth, the ensuing gradient of mean molecular weight has
relatively few dynamical consequences because N$_{2}$ is heavier
than water vapor, so that only the release of latent heat significantly
impacts convection. On the contrary, in a hydrogen dominated atmosphere
(e.g., giant planets), all condensing species are significantly heavier
than the background gas. This can stabilize the atmosphere against
convection near a cloud deck if the enrichment in the given species
exceeds a critical threshold. This raises two questions. What is
transporting energy in such a stabilized layer, and how affected can the
thermal profile of giant planets be? To answer these questions, we first
carry out a linear analysis of the convective and double-diffusive
instabilities in a condensable medium showing that an efficient
condensation can suppress double-diffusive convection. This suggests
that a stable radiative layer can form near a cloud condensation level,
leading to an increase in the temperature of the deep adiabat. Then, we
investigate the impact of the condensation of the most abundant species
(water) with a steady-state atmosphere model. Compared to standard
models, the temperature increase can reach several hundred degrees at
the quenching depth of key chemical tracers. Overall, this effect could
have many implications for our understanding of the dynamical and
chemical state of the atmosphere of giant planets, for their future
observations (with Juno for example), and for their internal evolution.
}},
doi = {10.1051/0004-6361/201629140},
adsurl = {https://ui.adsabs.harvard.edu/abs/2017A%26A...598A..98L},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017A_26A...598A..98L.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017A_26A...598A..98L.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2017MNRAS.464.3728B,
author = {{Bolmont}, E. and {Selsis}, F. and {Owen}, J.~E. and {Ribas}, I. and
{Raymond}, S.~N. and {Leconte}, J. and {Gillon}, M.},
title = {{Water loss from terrestrial planets orbiting ultracool dwarfs: implications for the planets of TRAPPIST-1}},
journal = {\mnras},
archiveprefix = {arXiv},
eprint = {1605.00616},
primaryclass = {astro-ph.EP},
keywords = {planets and satellites: atmospheres, planets and satellites: individual: TRAPPIST-1, planet star interactions, brown dwarfs, stars: low-mass},
year = 2017,
volume = 464,
pages = {3728-3741},
abstract = {{Ultracool dwarfs (UCD; T$_{eff}$ $\lt$ {\tilde}3000 K) cool to
settle on the main sequence after {\tilde}1 Gyr. For brown dwarfs, this
cooling never stops. Their habitable zones (HZ) thus sweeps inward at
least during the first Gyr of their lives. Assuming they possess water,
planets found in the HZ of UCDs have experienced a runaway greenhouse
phase too hot for liquid water prior to enter the HZ. It has been
proposed that such planets are desiccated by this hot early phase and
enter the HZ as dry worlds. Here, we model the water loss during this
pre-HZ hot phase taking into account recent upper limits on the XUV
emission of UCDs and using 1D radiation-hydrodynamic simulations. We
address the whole range of UCDs but also focus on the planets recently
found around the 0.08 M$_{&sun;}$ dwarf TRAPPIST-1. Despite
assumptions maximizing the FUV photolysis of water and the XUV-driven
escape of hydrogen, we find that planets can retain significant amount
of water in the HZ of UCDs, with a sweet spot in the 0.04-0.06
M$_{&sun;}$ range. We also studied the TRAPPIST-1 system using
observed constraints on the XUV flux. We find that TRAPPIST-1b and c may
have lost as much as 15 Earth oceans and planet d - which might be
inside the HZ - may have lost less than 1 Earth ocean. Depending on
their initial water contents, they could have enough water to remain
habitable. TRAPPIST-1 planets are key targets for atmospheric
characterization and could provide strong constraints on the water
erosion around UCDs.
}},
doi = {10.1093/mnras/stw2578},
adsurl = {https://ui.adsabs.harvard.edu/abs/2017MNRAS.464.3728B},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017MNRAS.464.3728B.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017MNRAS.464.3728B.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2017A&A...597A..94C,
author = {{Chiavassa}, A. and {Caldas}, A. and {Selsis}, F. and {Leconte}, J. and
{Von Paris}, P. and {Bordé}, P. and {Magic}, Z. and {Collet}, R. and
{Asplund}, M.},
title = {{Measuring stellar granulation during planet transits}},
journal = {\aap},
archiveprefix = {arXiv},
eprint = {1609.08966},
primaryclass = {astro-ph.EP},
keywords = {planet-star interactions, stars: activity, techniques: photometric, stars: atmospheres, hydrodynamics, radiative transfer},
year = 2017,
volume = 597,
eid = {A94},
pages = {A94},
abstract = {{Context. Stellar activity and convection-related surface structures
might cause bias in planet detection and characterization that use these
transits. Surface convection simulations help to quantify the
granulation signal.
Aims: We used realistic three-dimensional
(3D) radiative hydrodynamical (RHD) simulations from the Stagger grid
and synthetic images computed with the radiative transfer code Optim3D
to model the transits of three prototype planets: a hot Jupiter, a hot
Neptune, and a terrestrial planet.
Methods: We computed intensity
maps from RHD simulations of the Sun and a K-dwarf star at different
wavelength bands from optical to far-infrared that cover the range of
several ground- and space-based telescopes which observe exoplanet
transits. We modeled the transit using synthetic stellar-disk images
obtained with a spherical-tile imaging method and emulated the temporal
variation of the granulation intensity generating random images covering
a granulation time-series of 13.3 h. We measured the contribution of the
stellar granulation on the light curves during the planet transit.
Results: We identified two types of granulation noise that act
simultaneously during the planet transit: (I) the intrinsic change in
the granulation pattern with timescale (e.g., 10 min for solar-type
stars assumed in this work) is smaller than the usual planet transit (
hours as in our prototype cases); and (II) the fact that the transiting
planet occults isolated regions of the photosphere that differ in local
surface brightness as a result of convective-related surface structures.
First, we showed that our modeling approach returns granulation
timescale fluctuations that are comparable with what has been observed
for the Sun. Then, our statistical approach shows that the granulation
pattern of solar and K-dwarf-type stars have a non-negligible effect of
the light curve depth during the transit, and, consequentially on the
determination of the planet transit parameters such as the planet radius
(up to 0.90\% and 0.47\% for terrestrial and gaseous planets,
respectively). We also showed that larger (or smaller) orbital
inclination angles with respect to values corresponding to transit at
the stellar center display a shallower transit depth and longer ingress
and egress times, but also granulation fluctuations that are correlated
to the center-to-limb variation: they increase (or decrease) the value
of the inclination, which amplifies the fluctuations. The granulation
noise appears to be correlated among the different wavelength ranges
either in the visible or in the infrared regions.
Conclusions:
The prospects for planet detection and characterization with transiting
methods are excellent with access to large amounts of data for stars.
The granulation has to be considered as an intrinsic uncertainty (as a
result of stellar variability) on the precise measurements of exoplanet
transits of planets. The full characterization of the granulation is
essential for determining the degree of uncertainty on the planet
parameters. In this context, the use of 3D RHD simulations is important
to measure the convection-related fluctuations. This can be achieved by
performing precise and continuous observations of stellar photometry and
radial velocity, as we explained with RHD simulations, before, after,
and during the transit periods.
}},
doi = {10.1051/0004-6361/201528018},
adsurl = {https://ui.adsabs.harvard.edu/abs/2017A%26A...597A..94C},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017A_26A...597A..94C.pdf},
localpdf = {https://ui.adsabs.harvard.edu/abs/2017A_26A...597A..94C.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}