930 research outputs found
The effect of stellar limb darkening values on the accuracy of the planet radii derived from photometric transit observations
We study how the precision of the exoplanet radius determination is affected
by our present knowledge of limb darkening in two cases: when we fix the limb
darkening coefficients and when we adjust them. We also investigate the effects
of spots in one-colour photometry. We study the effect of limb darkening on the
planetary radius determination both via analytical expressions and by numerical
experiments. We also compare some of the existing limb darkening tables. When
stellar spots affect the fit, we replace the limb darkening coefficients,
calculated for the unspotted cases, with effective limb darkening coefficients
to describe the effect of the spots. There are two important cases. (1) When
one fixes the limb darkening values according to some theoretical predictions,
the inconsistencies of the tables do not allow us to reach accuracy in the
planetary radius of better than 1-10% (depending on the impact parameter) if
the host star's surface effective temperature is higher than 5000 K. Below 5000
K the radius ratio determination may contain even 20% error. (2) When one
allows adjustment of the limb darkening coefficients, the a/Rs ratio, the
planet-to-stellar radius ratio, and the impact parameter can be determined with
sufficient accuracy (<1%), if the signal-to-noise ratio is high enough.
However, the presence of stellar spots and faculae can destroy the agreement
between the limb darkening tables and the fitted limb darkening coefficients,
but this does not affect the precision of the planet radius determination. We
also find that it is necessary to fit the contamination factor, too. We
conclude that the present inconsistencies of theoretical stellar limb darkening
tables suggests one should not fix the limb darkening coefficients. When one
allows them to be adjusted, then the planet radius, impact parameter, and the
a/Rs can be obtained with the required precision.Comment: Astronomy & Astrophysics Vol. 549, A9 (2013) - 11 page
Estimating precipitation on early Mars using a radiative-convective model of the atmosphere and comparison with inferred runoff from geomorphology
We compare estimates of atmospheric precipitation during the Martian
Noachian-Hesperian boundary 3.8 Gyr ago as calculated in a radiative-convective
column model of the atmosphere with runoff values estimated from a
geomorphological analysis of dendritic valley network discharge rates. In the
atmospheric model, we assume CO2-H2O-N2 atmospheres with surface pressures
varying from 20 mb to 3 bar with input solar luminosity reduced to 75% the
modern value.
Results from the valley network analysis are of the order of a few mm d-1
liquid water precipitation (1.5-10.6 mm d-1, with a median of 3.1 mm d-1).
Atmospheric model results are much lower, from about 0.001-1 mm d-1 of snowfall
(depending on CO2 partial pressure). Hence, the atmospheric model predicts a
significantly lower amount of precipitated water than estimated from the
geomorphological analysis. Furthermore, global mean surface temperatures are
below freezing, i.e. runoff is most likely not directly linked to
precipitation. Therefore, our results strongly favor a cold early Mars with
episodic snowmelt as a source for runoff.
Our approach is challenged by mostly unconstrained parameters, e.g.
greenhouse gas abundance, global meteorology (for example, clouds) and
planetary parameters such as obliquity- which affect the atmospheric result -
as as well as by inherent problems in estimating discharge and runoff on
ancient Mars, such as a lack of knowledge on infiltration and evaporation rates
and on flooding timescales, which affect the geomorphological data.
Nevertheless, our work represents a first step in combining and interpreting
quantitative tools applied in early Mars atmospheric and geomorphological
studies.Comment: accepted in Planetary and Space Science, 37 pages, 14 figures, 2
table
A study of the performance of the transit detection tool DST in space-based surveys. Application of the CoRoT pipeline to Kepler data
Context. Transit detection algorithms are mathematical tools used for
detecting planets in the photometric data of transit surveys. In this work we
study their application to space-based surveys. Aims: Space missions are
exploring the parameter space of the transit surveys where classical algorithms
do not perform optimally, either because of the challenging signal-to-noise
ratio of the signal or its non-periodic characteristics. We have developed an
algorithm addressing these challenges for the mission CoRoT. Here we extend the
application to the data from the space mission Kepler. We aim at understanding
the performances of algorithms in different data sets. Methods: We built a
simple analytical model of the transit signal and developed a strategy for the
search that improves the detection performance for transiting planets. We
analyzed Kepler data with a set of stellar activity filtering and transit
detection tools from the CoRoT community that are designed for the search of
transiting planets. Results: We present a new algorithm and its performances
compared to one of the most widely used techniques in the literature using
CoRoT data. Additionally, we analyzed Kepler data corresponding to quarter Q1
and compare our results with the most recent list of planetary candidates from
the Kepler survey. We found candidates that went unnoticed by the Kepler team
when analyzing longer data sets. We study the impact of instrumental features
on the production of false alarms and false positives. These results show that
the analysis of space mission data advocates the use of complementary
detrending and transit detection tools also for future space-based transit
surveys such as PLATO.Comment: 18 pages, 23 figures, published in A&A, solved issue with reference
Estimating the number of planets that PLATO can detect
The PLATO mission is scheduled for launch in 2026. This study aims to
estimate the number of exoplanets that PLATO can detect as a function of
planetary size and period, stellar brightness, and observing strategy options.
Deviations from these estimates will be informative of the true occurrence
rates of planets, which helps constraining planet formation models. For this
purpose, we developed the Planet Yield for PLATO estimator (PYPE), which adopts
a statistical approach. We apply given occurrence rates from planet formation
models and from different search and vetting pipelines for the Kepler data. We
estimate the stellar sample to be observed by PLATO using a fraction of the
all-sky PLATO stellar input catalog (PIC). PLATO detection efficiencies are
calculated under different assumptions that are presented in detail in the
text. The results presented here primarily consider the current baseline
observing duration of four years. We find that the expected PLATO planet yield
increases rapidly over the first year and begins to saturate after two years. A
nominal (2+2) four-year mission could yield about several thousand to several
tens of thousands of planets, depending on the assumed planet occurrence rates.
We estimate a minimum of 500 Earth-size (0.8-1.25 RE) planets, about a dozen of
which would reside in a 250-500d period bin around G stars. We find that
one-third of the detected planets are around stars bright enough (V )
for RV-follow-up observations. We find that a three-year-long observation
followed by 6 two-month short observations (3+1 years) yield roughly twice as
many planets as two long observations of two years (2+2 years). The former
strategy is dominated by short-period planets, while the latter is more
beneficial for detecting earths in the habitable zone.Comment: 14 pages, 11 figures, accepted by A&A (July 5, 2023
Detectability of atmospheric features of Earth-like planets in the habitable zone around M dwarfs
We investigate the detectability of atmospheric spectral features of
Earth-like planets in the habitable zone (HZ) around M dwarfs with the future
James Webb Space Telescope (JWST). We use a coupled 1D climate-chemistry-model
to simulate the influence of a range of observed and modelled M-dwarf spectra
on Earth-like planets. The simulated atmospheres served as input for the
calculation of the transmission spectra of the hypothetical planets, using a
line-by-line spectral radiative transfer model. To investigate the
spectroscopic detectability of absorption bands with JWST we further developed
a signal-to-noise ratio (S/N) model and applied it to our transmission spectra.
High abundances of CH and HO in the atmosphere of Earth-like planets
around mid to late M dwarfs increase the detectability of the corresponding
spectral features compared to early M-dwarf planets. Increased temperatures in
the middle atmosphere of mid- to late-type M-dwarf planets expand the
atmosphere and further increase the detectability of absorption bands. To
detect CH, HO, and CO in the atmosphere of an Earth-like planet
around a mid to late M dwarf observing only one transit with JWST could be
enough up to a distance of 4 pc and less than ten transits up to a distance of
10 pc. As a consequence of saturation limits of JWST and less pronounced
absorption bands, the detection of spectral features of hypothetical Earth-like
planets around most early M dwarfs would require more than ten transits. We
identify 276 existing M dwarfs (including GJ 1132, TRAPPIST-1, GJ 1214, and LHS
1140) around which atmospheric absorption features of hypothetical Earth-like
planets could be detected by co-adding just a few transits. We show that using
transmission spectroscopy, JWST could provide enough precision to be able to
partly characterise the atmosphere of Earth-like TESS planets around mid to
late M dwarfs.Comment: 18 pages, 10 figure
Nonlinear Polariton Fluids in a Flatband Reveal Discrete Gap Solitons
Phase frustration in periodic lattices is responsible for the formation of
dispersionless flat bands. The absence of any kinetic energy scale makes flat
band physics critically sensitive to perturbations and interactions. We report
here on the experimental investigation of the nonlinear dynamics of cavity
polaritons in the gapped flat band of a one-dimensional Lieb lattice. We
observe the formation of gap solitons with quantized size and very abrupt
edges, signature of the frozen propagation of switching fronts. This type of
gap solitons belongs to the class of truncated Bloch waves, and had only been
observed in closed systems up to now. Here the driven-dissipative character of
the system gives rise to a complex multistability of the nonlinear domains
generated in the flat band. These results open up interesting perspective
regarding more complex 2D lattices and the generation of correlated photon
phases.Comment: 6 pages, 4 figures + supplemental material (6 pages, 6 figures
The extrasolar planet Gliese 581 d: a potentially habitable planet? (Corrigendum to arXiv:1009.5814)
We report here that the equation for H2O Rayleigh scattering was incorrectly
stated in the original paper [arXiv:1009.5814]. Instead of a quadratic
dependence on refractivity r, we accidentally quoted an r^4 dependence. Since
the correct form of the equation was implemented into the model, scientific
results are not affected.Comment: accepted to Astronomy&Astrophysic
Earth-like Habitats in Planetary Systems
Understanding the concept of habitability is related to an evolutionary
knowledge of the particular planet-in-question. Additional indications
so-called "systemic aspects" of the planetary system as a whole governs a
particular planet's claim on habitability. Here we focus on such systemic
aspects and discuss their relevance to the formation of an 'Earth-like'
habitable planet. We summarize our results obtained by lunar sample work and
numerical models within the framework of the Research Alliance "Planetary
Evolution and Life". We consider various scenarios which simulate the dynamical
evolution of the Solar System and discuss the likelihood of forming an
Earth-like world orbiting another star. Our model approach is constrained by
observations of the modern Solar System and the knowledge of its history.
Results suggest that the long-term presence of terrestrial planets is
jeopardized due to gravitational interactions if giant planets are present. But
habitability of inner rocky planets may be supported in those planetary systems
hosting giant planets.
Gravitational interactions within a complex multiple-body structure including
giant planets may supply terrestrial planets with materials which formed in the
colder region of the proto-planetary disk. During these processes, water, the
prime requisite for habitability, is delivered to the inner system. This may
occur either during the main accretion phase of terrestrial planets or via
impacts during a post-accretion bombardment. Results for both processes are
summarized and discussed with reference to the lunar crater record.
Starting from a scenario involving migration of the giant planets this
contribution discusses the delivery of water to Earth, the modification of
atmospheres by impacts in a planetary system context and the likelihood of the
existence of extrasolar Earth-like habitable worlds.Comment: 36 Pages, 6 figures, 2014, Special Issue in Planetary and Space
Science on the Helmholtz Research Alliance on Planetary Evolution and Lif
- …