592 research outputs found
The occurrence of planets and other substellar bodies around white dwarfs using K2
The majority of stars both host planetary systems and evolve into a white
dwarf (WD). To understand their post-main-sequence (PMS) planetary system
evolution, we present a search for transiting/eclipsing planets and other
Substellar Bodies (SBs) around WDs using a sample of 1148 WDs observed by K2.
Using transit injections, we estimate the completeness of our search. We place
constraints on the occurrence of planets and substellar bodies around white
dwarfs as a function of planet radius and orbital period. For short-period ( days) small objects, from asteroid-sized to , these are
the strongest constraints known to date. We further constrain the occurrence of
hot Jupiters (), habitable zone Earth-sized planets (), and
disintegrating short-period planets (). We blindly recovered all
previously known eclipsing objects, providing confidence in our analysis, and
make all light curves publicly available.Comment: Accepted by MNRA
Orbital Circularization of Hot and Cool Kepler Eclipsing Binaries
The rate of tidal circularization is predicted to be faster for relatively
cool stars with convective outer layers, compared to hotter stars with
radiative outer layers. Observing this effect is challenging, because it
requires large and well-characterized samples including both hot and cool
stars. Here we seek evidence for the predicted dependence of circularization
upon stellar type, using a sample of 945 eclipsing binaries observed by Kepler.
This sample complements earlier studies of this effect, which employed smaller
samples of better-characterized stars. For each Kepler binary we measure
based on the relative timing of the primary and secondary
eclipses. We examine the distribution of as a function of period
for binaries composed of hot stars, cool stars, and mixtures of the two types.
At the shortest periods, hot-hot binaries are most likely to be eccentric; for
periods shorter than 4 days, significant eccentricities occur frequently for
hot-hot binaries, but not for hot-cool or cool-cool binaries. This is in
qualitative agreement with theoretical expectations based on the slower
dissipation rates of hot stars. However, the interpretation of our results is
complicated by the largely unknown ages and evolutionary states of the stars in
our sample.Comment: Accepted for publication in Ap
ECCENTRICITY FROM TRANSIT PHOTOMETRY: SMALL PLANETS IN KEPLER MULTI-PLANET SYSTEMS HAVE LOW ECCENTRICITIES
Solar system planets move on almost circular orbits. In strong contrast, many massive gas giant exoplanets travel on highly elliptical orbits, whereas the shape of the orbits of smaller, more terrestrial, exoplanets remained largely elusive. Knowing the eccentricity distribution in systems of small planets would be important as it holds information about the planet's formation and evolution, and influences its habitability. We make these measurements using photometry from the Kepler satellite and utilizing a method relying on Kepler's second law, which relates the duration of a planetary transit to its orbital eccentricity, if the stellar density is known. Our sample consists of 28 bright stars with precise asteroseismic density measurements. These stars host 74 planets with an average radius of 2.6 R[subscript ⊕]. We find that the eccentricity of planets in Kepler multi-planet systems is low and can be described by a Rayleigh distribution with σ = 0.049 ± 0.013. This is in full agreement with solar system eccentricities, but in contrast to the eccentricity distributions previously derived for exoplanets from radial velocity studies. Our findings are helpful in identifying which planets are habitable because the location of the habitable zone depends on eccentricity, and to determine occurrence rates inferred for these planets because planets on circular orbits are less likely to transit. For measuring eccentricity it is crucial to detect and remove Transit Timing Variations (TTVs), and we present some previously unreported TTVs. Finally transit durations help distinguish between false positives and true planets and we use our measurements to confirm six new exoplanets.European Research Council (ASTERISK Project Grant Agreement 267864
A deep radius valley revealed by Kepler short cadence observations
The characteristics of the radius valley, i.e. an observed lack of planets between 1.5 and 2 Earth radii at periods shorter than
about 100 d, provide insights into the formation and evolution of close-in planets. We present a novel view of the radius valley
by refitting the transits of 431 planets using Kepler 1-min short cadence observations, the vast majority of which have not been
previously analysed in this way. In some cases, the updated planetary parameters differ significantly from previous studies,
resulting in a deeper radius valley than previously observed. This suggests that planets are likely to have a more homogeneous
core composition at formation. Furthermore, using support vector machines, we find that the radius valley location strongly
depends on orbital period and stellar mass and weakly depends on stellar age, with ∂ log
Rp,valley
/∂ log P = −0.096+0.023 −0.027,
∂ log
Rp,valley
/∂ log M = 0.231+0.053 −0.064, and ∂ log
Rp,valley
/∂ log (age) = 0.033+0.017
−0.025. These findings favour thermally driven
mass-loss models such as photoevaporation and core-powered mass-loss, with a slight preference for the latter scenario. Finally,
this work highlights the value of transit observations with a short photometric cadence to precisely determine planet radii, and
we provide an updated list of precisely and homogeneously determined parameters for the planets in our sample
The occurrence rate of giant planets orbiting low-mass stars with TESS
We present a systematic search for transiting giant planets () orbiting nearby low-mass stars (). The formation of giant planets around low-mass stars is
predicted to be rare by the core-accretion planet formation theory. We search
91,306 low-mass stars in the TESS 30 minute cadence photometry detecting
fifteen giant planet candidates, including seven new planet candidates which
were not known planets or identified as TOIs prior to our search. Our
candidates present an exciting opportunity to improve our knowledge of the
giant planet population around the lowest mass stars. We perform planet
injection-recovery simulations and find that our pipeline has a high detection
efficiency across the majority of our targeted parameter space. We measure the
occurrence rates of giant planets with host stars in different stellar mass
ranges spanning our full sample. We find occurrence rates of %
(0.088 - 0.26 ), % (0.26 - 0.42 ), and
% (0.42 - 0.71 ). For our full sample (0.088 - 0.71
) we find a giant planet occurrence rate of %. We
have measured for the first time the occurrence rate for giant planets orbiting
stars with and we demonstrate this occurrence rate
to be non-zero. This result contradicts currently accepted planet formation
models and we discuss some possibilities for how these planets could have
formed.Comment: 20 pages, 14 figures. Accepted for publication in MNRA
Understanding and predicting cadence effects in the characterization of exoplanet transits
We investigate the effect of observing cadence on the precision of radius ratio values obtained from transit light curves by performing uniform Markov chain Monte Carlo fits of 46 exoplanets observed by the Transiting Exoplanet Survey Satellite (TESS) in multiple cadences. We find median improvements of almost 50 per cent when comparing fits to 20 and 120 s cadence light curves to 1800 s cadence light curves, and of 37 per cent when comparing 600 s cadence to 1800 s cadence. Such improvements in radius precision are important, for example, to precisely constrain the properties of the radius valley or to characterize exoplanet atmospheres. We also implement a numerical information analysis to predict the precision of parameter estimates for different observing cadences. We tested this analysis on our sample and found that it reliably predicts the effect of shortening observing cadence with errors in the predicted percentage precision of for most cases. We apply this method to 157 TESS objects of interest that have only been observed with 1800 s cadence to predict the precision improvement that could be obtained by reobservations with shorter cadences and provide the full table of expected improvements. We report the 10 planet candidates that would benefit the most from reobservations at short cadence. Our implementation of the information analysis for the prediction of the precision of exoplanet parameters, Prediction of Exoplanet Precisions using Information in Transit Analysis, is made publicly available
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