Kepler-503b: An Object at the Hydrogen Burning Mass Limit Orbiting a Subgiant Star

Cañas, Caleb I.; Bender, Chad F.; Mahadevan, Suvrath; Fleming, Scott W.; Beatty, Thomas G.; Covey, Kevin R.; Lee, Nathan De; Hearty, Fred; García-Hernández, D. A.; Majewski, Steven R.; Schneider, Donald P.; Stassun, Keivan G.; Wilson, R.

doi:10.3847/2041-8213/aacbc5

Cited by 22 publications

(17 citation statements)

References 46 publications

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“…Recently, a possible substellar object orbiting the solar-like contact binary V2284 Cyg was first reported by Wang et al (2017), and also in the K-type shallow contact binary CC Com with very low mass M 3 = 0.066 M by Yang et al (2009a), and KIC 9532219 with M 3 = 0.089 M by Lee et al (2016) or TX Cnc with M 3 = 0.097 M by Liu et al (2007). More recently, the eclipsing binary Kepler-503 has been found to be a brown dwarf or low-mass star with M 3 = 0.075 M orbiting around a subgiant star (Cañas et al 2018). Therefore, the existence of a third body in the system cannot be ruled out completely.…”

Section: Discussionmentioning

confidence: 97%

RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

Sarotsakulchai

Qian

Soonthornthum

et al. 2019

Publications of the Astronomical Society of Japan

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New CCD photometric light curves of the short-period (P = 0.285 d) eclipsing binary RW Dor are presented. The observations were performed with the PROMPT-8 robotic telescope at CTIO in Chile between 2015 March and 2017 March. Other eclipse timings were obtained from the 2.15 m JS telescope at CASLEO, San Juan, Argentina in 2011 December. Based on a light curve analysis, it is found that RW Dor is a W-type shallow contact binary with a fill-out factor f ∼ 11% and a high mass ratio q ∼ 1.587 (1/q = 0.63), where the hotter component is the less massive one (M 1 ∼ 0.52 M and M 2 ∼ 0.82 M ). For orbital-period investigation, 15 new eclipse times and those previously published were compiled. O − C analysis with very weak evidence suggests that a long-term decrease in period with a rate of dP/dt = −9.61 × 10 −9 d yr −1 is superimposed on a cyclic variation (A 3 = 0.0054 d and P 3 = 49.9 yr). The long-term decrease can be interpreted as mass transfer from the more massive component to the less massive one, or combined with angular momentum loss via magnetic braking. In addition, the marginal contact phase, high mass ratio (1/q > 0.4), and long-term decrease in period all suggest that RW Dor is a newly formed contact binary via Case A mass transfer, and it will evolve into a deeper normal contact binary. If the cyclic change is correct, the light travel-time effect via the presence of a cool third body will be a more plausible explanation for this.

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Section: Discussionmentioning

confidence: 97%

RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

Sarotsakulchai

Qian

Soonthornthum

et al. 2019

Publications of the Astronomical Society of Japan

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“…Whereas brown dwarfs detected only with radial velocities do not have clearly defined upper mass limits and may actually be low-mass stars (e.g., Kiefer et al 2021). Space-based photometric missions are ideal to find these rare objects given their robust photometric precision and long uninterrupted observations, and recent missions such as Kepler (Borucki et al 2010) and K2 (Howell et al 2014) have led to successful follow-up mass measurements of transiting brown dwarfs (e.g., Bayliss et al 2017;Cañas et al 2018;Carmichael et al 2019;Persson et al 2019). The currently operating space-based all-sky Transiting Exoplanet Survey Satellite (TESS; Ricker et al 2015) has continued to populate the sparse desert with well-characterized brown dwarfs and very low-mass stars (e.g., Šubjak et al 2020;Carmichael et al 2020Carmichael et al , 2021Mireles et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Populating the brown dwarf and stellar boundary: Five stars with transiting companions near the hydrogen-burning mass limit

Grieves

Bouchy

Lendl

et al. 2021

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Where a licence is displayed above, please note the terms and conditions of the licence govern your use of this document.When citing, please reference the published version. Take down policyWhile the University of Birmingham exercises care and attention in making items available there are rare occasions when an item has been uploaded in error or has been deemed to be commercially or otherwise sensitive.

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“…Later discoveries of six additional BDs have been made from space: Kepler-503b (Cañas et al 2018), EPIC 219388192b (Nowak et al 2017), EPIC 201702477b (Bayliss et al 2017), and from the ground: WASP-128b (Hodžić et al 2018), LP 261-75b (Irwin et al 2018), and HATS-70b (Zhou et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Greening of the brown-dwarf desert

Persson

Csizmadia

Mustill

et al. 2019

A&A

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Context. Although more than 2000 brown dwarfs have been detected to date, mainly from direct imaging, their characterisation is difficult due to their faintness and model-dependent results. In the case of transiting brown dwarfs, however, it is possible to make direct high-precision observations. Aims. Our aim is to investigate the nature and formation of brown dwarfs by adding a new well-characterised object, in terms of its mass, radius and bulk density, to the currently small sample of less than 20 transiting brown dwarfs. Methods. One brown dwarf candidate was found by the KESPRINT consortium when searching for exoplanets in the K2 space mission Campaign 16 field. We combined the K2 photometric data with a series of multicolour photometric observations, imaging, and radial velocity measurements to rule out false positive scenarios and to determine the fundamental properties of the system. Results. We report the discovery and characterisation of a transiting brown dwarf in a 5.17-day eccentric orbit around the slightly evolved F7 V star EPIC 212036875. We find a stellar mass of 1.15 ± 0.08 M⊙, a stellar radius of 1.41 ± 0.05 R⊙, and an age of 5.1 ± 0.9 Gyr. The mass and radius of the companion brown dwarf are 51 ± 2 MJ and 0.83 ± 0.03 RJ, respectively, corresponding to a mean density of 108−13+15 g cm−3. Conclusions. EPIC 212036875 b is a rare object that resides in the brown-dwarf desert. In the mass-density diagram for planets, brown dwarfs, and stars, we find that all giant planets and brown dwarfs follow the same trend from ~0.3 MJ to the turn-over to hydrogen burning stars at ~ 73 MJ. EPIC 212036875 b falls close to the theoretical model for mature H/He dominated objects in this diagram as determined by interior structure models. We argue that EPIC 212036875 b formed via gravitational disc instabilities in the outer part of the disc, followed by a quick migration. Orbital tidal circularisation may have started early in its history for a brief period when the brown dwarf’s radius was larger. The lack of spin–orbit synchronisation points to a weak stellar dissipation parameter (Q⋆′ ≳ 108), which implies a circularisation timescale of ≳23 Gyr, or suggests an interaction between the magnetic and tidal forces of the star and the brown dwarf.

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Kepler-503b: An Object at the Hydrogen Burning Mass Limit Orbiting a Subgiant Star

Cited by 22 publications

References 46 publications

RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

Populating the brown dwarf and stellar boundary: Five stars with transiting companions near the hydrogen-burning mass limit

Greening of the brown-dwarf desert

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