Measuring the rotation period distribution of field M dwarfs with Kepler

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

doi:10.1093/mnras/stt536

Cited by 426 publications

(500 citation statements)

References 45 publications

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“…This is due to an age difference between the two samples, since the Glebocki and Gnacinski (2005) catalog mainly consists of young open cluster stars. However, our results for Mtype stars agree well with those reported by Reiners and Mohanty (2012) and McQuillan et al (2013). The study by Debosscher et al (2011) analyzed a different set of Kepler data, but we still find good agreement with the stars overlapping with our sample.…”

Section: Discussionsupporting

confidence: 91%

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Differential Rotation in Sun-like Stars from Surface Variability and Asteroseismology

Nielsen

2017

Springer Theses

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Section: Discussionsupporting

confidence: 91%

“…Figure 2.3 shows the distributions of stars that have been classified as M-type, found in this work and those by McQuillan et al (2013). The median of the distribution in our sample is 15.4 days.…”

Section: Rotation Of Late Type Starsmentioning

confidence: 70%

Differential Rotation in Sun-like Stars from Surface Variability and Asteroseismology

Nielsen

2017

Springer Theses

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“…The most striking feature is the presence of two distinct branches separated by the, so called, Vaughan-Preston gap (Vaughan & Preston 1980). Many explanations have been proposed to explain the gap including different dynamos operating along each branch (Böhm-Vitense 2007), an abrupt change in chromospheric activity with stellar age (Pace et al 2009), or multiple waves of star formation (McQuillan et al 2013).…”

Section: Observing Earth-analoguesmentioning

confidence: 99%

The effects of stellar winds on the magnetospheres and potential habitability of exoplanets

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Jardine

Vidotto

et al. 2014

A&A

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Context. The principle definition of habitability for exoplanets is whether they can sustain liquid water on their surfaces, i.e. that they orbit within the habitable zone. However, the planet's magnetosphere should also be considered, since without it, an exoplanet's atmosphere may be eroded away by stellar winds. Aims. The aim of this paper is to investigate magnetospheric protection of a planet from the effects of stellar winds from solar-mass stars. Methods. We study hypothetical Earth-like exoplanets orbiting in the host star's habitable zone for a sample of 124 solar-mass stars. These are targets that have been observed by the Bcool Collaboration. Using two wind models, we calculate the magnetospheric extent of each exoplanet. These wind models are computationally inexpensive and allow the community to quickly estimate the magnetospheric size of magnetised Earth-analogues orbiting cool stars. Results. Most of the simulated planets in our sample can maintain a magnetosphere of ∼5 Earth radii or larger. This suggests that magnetised Earth analogues in the habitable zones of solar analogues are able to protect their atmospheres and is in contrast to planets around young active M dwarfs. In general, we find that Earth-analogues around solar-type stars, of age 1.5 Gyr or older, can maintain at least a Paleoarchean Earth sized magnetosphere. Our results indicate that planets around 0.6-0.8 solar-mass stars on the low activity side of the Vaughan-Preston gap are the optimum observing targets for habitable Earth analogues.

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“…As an additional verification, we also computed the light curve autocorrelation (McQuillan et al 2013 The green dotted lines indicate the center of Gaussians fitted to the data to derive the main frequency and its harmonics. The vertical red line corresponds to the rotation period deduced from the v sin i and the star's radius, assuming the star's rotation axis is perpendicular to the line of sight, and the shaded areas are the associated 1σ, 2σ, and 3σ upper limit regions from the darkest to the lightest one.…”

Section: Kepler Photometric Observationsmentioning

confidence: 99%

SOPHIE velocimetry ofKeplertransit candidates XI. Kepler-412 system: probing the properties of a new inflated hot Jupiter

Deleuil

Almenara

Santerne

et al. 2014

A&A

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Context. Hot Jupiters are still a fascinating exoplanet population that presents a diversity we are still far from understanding. Highprecision photometric observations combined with radial velocity measurements give us a unique opportunity to constrain their properties better, on both their internal structure and their atmospheric bulk properties. Aims. We initiated a follow-up program of Kepler-released planet candidates with the goal of confirming the planetary nature of a number of them through radial velocity measurements. For those that successfully passed the radial velocity screening, we furthermore performed a detailed exploration of their properties to characterize the systems. As a byproduct, these systematic observations allow us to consolidate the exoplanets' occurrence rate. Methods. We performed a complete analysis of the Kepler-412 system, listed as planet candidate KOI-202 in the Kepler catalog, by combining the Kepler observations from Q1 to Q15, to ground-based spectroscopic observations that allowed us to derive radial velocity measurements, together with the host-star parameters and properties. We also analyzed the light curve to derive the star's rotation period and the phase function of the planet, including the secondary eclipse. Results. We secured the planetary nature of Kepler-412b. We found the planet has a mass of 0.939 ± 0.085 M Jup and a radius of 1.325 ± 0.043 R Jup , which makes it a member of the bloated giant subgroup. It orbits its G3 V host star in 1.72 days. The system has an isochronal age of 5.1 Gyr, consistent with its moderate stellar activity as observed in the Kepler light curve and the rotation of the star of 17.2 ± 1.6 days. From the detected secondary we derived the day-side temperature as a function of the geometric albedo. We estimated that the geometrical albedo A g should be between 0.094 ± 0.015 and 0.013 +0.017 −0.013 and the brightness of the day side 2380 ± 40 K. The measured night-side flux corresponds to a night-side brightness temperature of 2154 ± 83 K, much greater than what is expected for a planet with homogeneous heat redistribution. From the comparison to star and planet evolution models, we found that dissipation should operate in the deep interior of the planet. This modeling also shows that despite its inflated radius, the planet presents a noticeable amount of heavy elements, which accounts for a mass fraction of 0.11 ± 0.04.

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Measuring the rotation period distribution of field M dwarfs with Kepler

Cited by 426 publications

References 45 publications

Differential Rotation in Sun-like Stars from Surface Variability and Asteroseismology

Differential Rotation in Sun-like Stars from Surface Variability and Asteroseismology

The effects of stellar winds on the magnetospheres and potential habitability of exoplanets

SOPHIE velocimetry ofKeplertransit candidates XI. Kepler-412 system: probing the properties of a new inflated hot Jupiter

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