LHS 6343 C: A TRANSITING FIELD BROWN DWARF DISCOVERED BY THE<i>KEPLER</i>MISSION

Johnson, John Asher; Apps, Kevin; Gazak, J. Zachary; Crepp, Justin R.; Crossfield, Ian J. M.; Howard, Andrew W.; Marcy, G. W.; Morton, Timothy; Chubak, Carly; Isaacson, Howard

doi:10.1088/0004-637x/730/2/79

Cited by 96 publications

(142 citation statements)

References 64 publications

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“…In our case, the parameters have been derived by Johnson et al (2011) by fitting the radial velocity and transit light-curves. Therefore, we can use their values and uncertainties to define the prior as…”

Section: Resultsmentioning

confidence: 99%

“…The two M-type components A and B of the visual binary, separated by 0. 55 (Johnson et al 2011), are contained inside a single pixel of the Kepler images (the pixel side being 3. 98), and hence any photometric mask selected for the A component contains contamination from component B. Co-trending basis vectors are applied to the raw data using the PyKE pipeline reduction software 1 to correct for systematic trends, which are mainly related to the pointing jitter of the satellite, detector instabilities, and environment variations (Murphy 2012).…”

Section: Photometrymentioning

confidence: 99%

“…Finally, eclipses were removed from the data set considering the ephemeris and the system parameters in Herrero et al (2013). A complete analysis of the photometry of the brown dwarf eclipses can be found in Johnson et al (2011) and Herrero et al (2013). The de-trended out-of-eclipse light curve is shown in Fig.…”

Section: Photometrymentioning

confidence: 99%

“…m is the mass of the brown dwarf secondary, M * the mass of the distorted primary star, R its radius, and i the inclination of the orbital plane, which are fixed to those derived by Johnson et al (2011). Finally, Z 1 (2) is a coefficient given by…”

Section: Models Of the Doppler-beaming And Ellipticity Effectmentioning

confidence: 99%

“…This eclipsing binary consists of an M4V star (component A) and a brown dwarf (62.7 M Jup , component C) and was discovered by Johnson et al (2011) as part of the system LHS 6343 AB, a visual binary consisting of two M-dwarf stars with a projected separation of 0. 55.…”

Section: Introductionmentioning

confidence: 99%

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Doppler-beaming in theKeplerlight curve of LHS 6343 A

Herrero¹,

Lanza²,

Ribas³

et al. 2014

A&A

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Context. Kepler observations revealed a brown dwarf eclipsing the M-type star LHS 6343 A with a period of 12.71 days. In addition, an out-of-eclipse light modulation with the same period and a relative semi-amplitude of ∼2 × 10 −4 was observed showing an almost constant phase lag to the eclipses produced by the brown dwarf. In a previous work, we concluded that this was due to the light modulation induced by photospheric active regions in LHS 6343 A. Aims. In the present work, we prove that most of the out-of-eclipse light modulation is caused by the Doppler-beaming induced by the orbital motion of the primary star. Methods. We introduce a model of the Doppler-beaming for an eccentric orbit and also considered the ellipsoidal effect. The data were fitted using a Bayesian approach implemented through a Markov chain Monte Carlo method. Model residuals were analysed by searching for periodicities using a Lomb-Scargle periodogram. Results. For the first seven quarters of Kepler observations and the orbit previously derived from the radial velocity measurements, we show that the light modulation of the system outside eclipses is dominated by the Doppler-beaming effect. A period search performed on the residuals shows a significant periodicity of 42.5 ± 3.2 days with a false-alarm probability of 5 × 10 −4 , probably associated with the rotational modulation of the primary component.

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Section: Resultsmentioning

confidence: 99%

Section: Photometrymentioning

confidence: 99%

Section: Photometrymentioning

confidence: 99%

Section: Models Of the Doppler-beaming And Ellipticity Effectmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Doppler-beaming in theKeplerlight curve of LHS 6343 A

Herrero¹,

Lanza²,

Ribas³

et al. 2014

A&A

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Brown dwarf characterization with EChO

et al. 2015

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Understanding exoplanet formation, structure and evolution in 2010

2010

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Abstract. In this short review, we summarize our present understanding (and non-understanding) of exoplanet formation, structure and evolution, in the light of the most recent discoveries. Recent observations of transiting massive brown dwarfs seem to remarkably confirm the predicted theoretical mass-radius relationship in this domain. This mass-radius relationship provides, in some cases, a powerful diagnostic to distinguish planets from brown dwarfs of same mass, as for instance for Hat-P-20b. If confirmed, this latter observation shows that planet formation takes place up to at least 8 Jupiter masses. Conversely, observations of brown dwarfs down to a few Jupiter masses in young, low-extinction clusters strongly suggests an overlapping mass domain between (massive) planets and (low-mass) brown dwarfs, i.e. no mass edge between these two distinct (in terms of formation mechanism) populations. At last, the large fraction of heavy material inferred for many of the transiting planets confirms the core-accretion scenario as been the dominant one for planet formation.Keywords. planets and satellites: general 1. Planet internal structure and evolution General overviewThe realm of extrasolar planet discoveries now extends from gaseous giants of several Jupiter masses down to objects of a few Earth masses. Detailed models of planet structure and evolution have been computed by different groups (Fortney et al. 2007, Baraffe et al. 2008, Burrows et al. 2007 see Baraffe et al. 2010 for a recent review). These calculations include various internal compositions, based on presently available high-pressure equations of state (EOS) for materials typical of planetary interiors. A detailed discussion and a comparison of these models can be found in Baraffe et al. (2008) †. This latter paper also explores the effect of the location of the heavy element material in the planet, either all gathered at depth as a central core or distributed throughout the gaseous H/He envelope, on the planet's radius evolution. These different possible distributions of heavy elements can in some cases have an important impact on the planet's contraction. This paper also shows that the presence of even a modest gaseous (H/He) atmosphere hampers an accurate determination of the planet's internal composition, as the highly compressible gas contains most of the entropy of the planet and thus governs its cooling and contraction rate. In such cases, only the average internal composition of the planet can be inferred from a comparison of the models with the observed mass and radius determinations, for transiting objects. † Models are available at

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LHS 6343 C: A TRANSITING FIELD BROWN DWARF DISCOVERED BY THEKEPLERMISSION

Cited by 96 publications

References 64 publications

Doppler-beaming in theKeplerlight curve of LHS 6343 A

Doppler-beaming in theKeplerlight curve of LHS 6343 A

Brown dwarf characterization with EChO

Understanding exoplanet formation, structure and evolution in 2010

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