STELLAR ROTATION PERIODS OF THE
                    <i>KEPLER</i>
                    OBJECTS OF INTEREST: A DEARTH OF CLOSE-IN PLANETS AROUND FAST ROTATORS

McQuillan, A.; Mazeh, T.; Aigrain, S.

doi:10.1088/2041-8205/775/1/l11

Cited by 258 publications

(294 citation statements)

References 37 publications

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“…We failed to find any close-in planet around fast-rotating stars, confirming the results obtained by McQuillan et al (2013b).…”

Section: Discussionsupporting

confidence: 91%

“…All of them are single systems to the best of our knowledge. By studying P rot as a function of the orbital period of the innermost planet, we found that there are no close-in planets around fast rotators in this small sample of asteroseismic targets, as pointed out by McQuillan et al (2013b). The study of the KOI light curves requires a specific analysis to properly remove the transit signature without affecting the rotation modulation.…”

Section: Discussionmentioning

confidence: 60%

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Rotation and magnetism ofKeplerpulsating solar-like stars

García

Ceillier

Salabert

et al. 2014

A&A

270

344

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Kepler ultra-high precision photometry of long and continuous observations provides a unique dataset in which surface rotation and variability can be studied for thousands of stars. Because many of these old field stars also have independently measured asteroseismic ages, measurements of rotation and activity are particularly interesting in the context of age-rotation-activity relations. In particular, age-rotation relations generally lack good calibrators at old ages, a problem that this Kepler sample of old-field stars is uniquely suited to address. We study the surface rotation and photometric magnetic activity of a subset of 540 solar-like stars on the mainsequence and the subgiant branch for which stellar pulsations have been measured. The rotation period was determined by comparing the results from two different analysis methods: i) the projection onto the frequency domain of the time-period analysis, and ii) the autocorrelation function of the light curves. Reliable surface rotation rates were then extracted by comparing the results from two different sets of calibrated data and from the two complementary analyses. General photometric levels of magnetic activity in this sample of stars were also extracted by using a photometric activity index, which takes into account the rotation period of the stars. We report rotation periods for 310 out of 540 targets (excluding known binaries and candidate planet-host stars); our measurements span a range of 1 to 100 days. The photometric magnetic activity levels of these stars were computed, and for 61.5% of the dwarfs, this level is similar to the range, from minimum to maximum, of the solar magnetic activity. We demonstrate that hot dwarfs, cool dwarfs, and subgiants have very different rotation-age relationships, highlighting the importance of separating out distinct populations when interpreting stellar rotation periods. Our sample of cool dwarf stars with age and metallicity data of the highest quality is consistent with gyrochronology relations reported in the literature.

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“…We failed to find any close-in planet around fast-rotating stars, confirming the results obtained by McQuillan et al (2013b).…”

Section: Discussionsupporting

confidence: 91%

Section: Discussionmentioning

confidence: 60%

Rotation and magnetism ofKeplerpulsating solar-like stars

García

Ceillier

Salabert

et al. 2014

A&A

270

344

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“…In the case of Kepler-49 c, the models and transit shape are consistent with a near-grazing (b∼0.9) model. The host is known to be an active star with a likely rotation period of∼18.5 days (McQuillan et al 2013). We speculate that Kepler-49 c was seen to be consistently crossing a polar star spot resulting in a diluted transit depth.…”

Section: Stellar Parametersmentioning

confidence: 84%

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M _⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES

Jontof-Hutter

Ford

Rowe

et al. 2016

ApJ

176

147

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We infer dynamical masses in eight multiplanet systems using transit times measured from Keplerʼs complete dataset, including short-cadence data where available. Of the 18dynamical masses that we infer, 10pass multiple tests for robustness. These are in systemsKepler-26 (KOI-250), Kepler-29 (KOI-738), Kepler-60 (KOI-2086), , and Kepler-307 (KOI-1576). Kepler-105 c has a radius of 1.3 R ⊕ and a density consistent with an Earth-like composition. Strong transit timing variation(TTV) signals were detected from additional planets, but their inferred masses were sensitive to outliers or consistent solutions could not be found with independently measured transit times, including planets orbitingKepler-49 (KOI-248), Kepler-57 (KOI-1270), Kepler-105 (KOI-115), and Kepler-177 (KOI-523). Nonetheless, strong upper limits on the mass of Kepler-177 c imply an extremely low density of∼0.1 g cm −3 . In most cases, individual orbital eccentricities were poorly constrained owingto degeneracies in TTV inversion. For five planet pairs in our sample, strong secular interactions imply a moderatetohigh likelihood of apsidal alignment over a wide range of possible eccentricities. We also find solutions for the three planets known to orbit Kepler-60 in a Laplace-like resonance chain. However, nonlibrating solutions also match the transittiming data. For six systems, we calculate more precise stellar parameters than previously known, enabling useful constraints on planetary densities where we have secure mass measurements. Placing these exoplanets on the mass-radius diagram, we find thata wide range of densities isobserved among sub-Neptune-mass planets and that the range in observed densities is anticorrelated with incident flux.

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“…In agreement, Walkowicz & Basri (2013) reported a rotation period of P = 33.26 ± 3.44 days for this star, based on the analysis of quarter 9 data alone. On the other hand, McQuillan et al (2013) did not find a significant period for this star from the auto-correlation function on quarter 3−14 data. This periodicity could be interpreted as the rotational period because it is present identically in the first and second halves of the light curve.…”

Section: Primary Star Parametersmentioning

confidence: 62%

SOPHIE velocimetry ofKeplertransit candidates

Díaz

Montagnier

Leconte

et al. 2014

A&A

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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 ± 0.0033 M and a radius R = 0.1025 ± 0.0024 R . 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 ± 0.0043 M ; R = 0.1201 ± 0.0033 R ), and its position in the mass-radius diagram agrees well with theoretical expectations.

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STELLAR ROTATION PERIODS OF THE KEPLER OBJECTS OF INTEREST: A DEARTH OF CLOSE-IN PLANETS AROUND FAST ROTATORS

Cited by 258 publications

References 37 publications

Rotation and magnetism ofKeplerpulsating solar-like stars

Rotation and magnetism ofKeplerpulsating solar-like stars

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M _⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES

SOPHIE velocimetry ofKeplertransit candidates

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STELLAR ROTATION PERIODS OF THE KEPLER OBJECTS OF INTEREST: A DEARTH OF CLOSE-IN PLANETS AROUND FAST ROTATORS

Cited by 258 publications

References 37 publications

Rotation and magnetism ofKeplerpulsating solar-like stars

Rotation and magnetism ofKeplerpulsating solar-like stars

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M ⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES

SOPHIE velocimetry ofKeplertransit candidates

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Product

Resources

About

SECURE MASS MEASUREMENTS FROM TRANSIT TIMING: 10 KEPLER EXOPLANETS BETWEEN 3 AND 8 M _⊕ WITH DIVERSE DENSITIES AND INCIDENT FLUXES