DISCOVERY OF A TRANSITING PLANET AND EIGHT ECLIPSING BINARIES IN HATNet FIELD G205

Latham, David W.; Bakos, G. Á.; Torres, Guillermo; Stefanik, R. P.; Noyes, R. W.; Kovács, G.; Pál, András; Marcy, Geoffrey W.; Fischer, Debra A.; Butler, R. Paul; Sipőcz, Brigitta; Sasselov, Dimitar; Esquerdo, Gilbert A.; Vogt, Steven S.; Hartman, J. D.; Kovács, G.; Lázár, J.; Papp, I.; Sári, P.

doi:10.1088/0004-637x/704/2/1107

Cited by 92 publications

(117 citation statements)

References 44 publications

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“…For HAT-P-8, an angular separation of 1.027 ′′ between HAT-P-8 and its stellar binary companion (Bergfors et al 2013) and a distance of 230 pc (Latham et al 2009) imply a projected separation of ≈ 236 AU. Eastman et al (2016) found a projected separation for KELT-4Ab of 328 AU.…”

Section: Constraints On Stellar Triples Hosting Hjs and Comparisons Tmentioning

confidence: 99%

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On the formation of hot and warm Jupiters via secular high-eccentricity migration in stellar triples

Hamers

2017

Mon. Not. R. Astron. Soc.

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Hot Jupiters (HJs) are Jupiter-like planets orbiting their host star in tight orbits of a few days. They are commonly believed not to have formed in situ, requiring inwards migration towards the host star. One of the proposed migration scenarios is secular high-eccentricity or high-e migration, in which the orbit of the planet is perturbed to high eccentricity by secular processes, triggering strong tidal evolution and orbital migration. Previous theoretical studies have considered secular excitation in stellar binaries. Recently, a number of HJs have been observed in stellar triple systems. In the latter, the secular dynamics are much richer compared to stellar binaries, and HJs could potentially be formed more efficiently. Here, we investigate this possibility by modeling the secular dynamical and tidal evolution of planets in two hierarchical configurations in stellar triple systems. We find that the HJ formation efficiency is higher compared to stellar binaries, but only by at most a few tens of per cent. The orbital properties of the HJs formed in the simulations are very similar to HJs formed in stellar binaries, and similarly to studies of the latter we find no significant number of warm Jupiters. HJs are only formed in our simulations for triples with specific orbital configurations, and our constraints are approximately consistent with current observations. In future, this allows to rule out high-e migration in stellar triples if a HJ is detected in a triple grossly violating these constraints.

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Section: Constraints On Stellar Triples Hosting Hjs and Comparisons Tmentioning

confidence: 99%

“…The three HJs are WASP-12b (Hebb et al 2009;Bergfors et al 2013;Bechter et al 2014), HAT-P-8b (Latham et al 2009;Bergfors et al 2013;Bechter et al 2014), and KELT-4Ab (Eastman et al 2016). In these systems, the HJs orbit the tertiary star in a stellar triple system, i.e.…”

Section: Introductionmentioning

confidence: 99%

On the formation of hot and warm Jupiters via secular high-eccentricity migration in stellar triples

Hamers

2017

Mon. Not. R. Astron. Soc.

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“…76 pixel −1 ) and the large proper motion on which our targets were selected (μ > 0. 15 yr −1 ; from Lépine & Shara 2005), blended background eclipsing binaries are not a significant source of false positives (see Latham et al 2009;Triaud et al 2013 for contrast).…”

Section: Observationsmentioning

confidence: 99%

Constraints on Planet Occurrence Around Nearby Mid-to-Late M Dwarfs From the Mearth Project

Berta

Irwin

Charbonneau

2013

ApJ

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The MEarth Project is a ground-based photometric survey intended to find planets transiting the closest and smallest main-sequence stars. In its first four years, MEarth discovered one transiting exoplanet, the 2.7 R ⊕ planet GJ1214b. Here, we answer an outstanding question: in light of the bounty of small planets transiting small stars uncovered by the Kepler mission, should MEarth have found more than just one planet so far? We estimate MEarth's ensemble sensitivity to exoplanets by performing end-to-end simulations of 1.25 × 10 6 observations of 988 nearby mid-tolate M dwarfs, gathered by MEarth between 2008 October and 2012 June. For 2-4 R ⊕ planets, we compare this sensitivity to results from Kepler and find that MEarth should have found planets at a rate of 0.05-0.36 planets yr −1 in its first four years. As part of this analysis, we provide new analytic fits to the Kepler early M dwarf planet occurrence distribution. When extrapolating between Kepler's early M dwarfs and MEarth's mid-to-late M dwarfs, we find that assuming the planet occurrence distribution stays fixed with respect to planetary equilibrium temperature provides a good match to our detection of a planet with GJ1214b's observed properties. For larger planets, we find that the warm (600-700 K), Neptune-sized (4 R ⊕ ) exoplanets that transit early M dwarfs like Gl436 and GJ3470 occur at a rate of <0.15 star −1 (at 95% confidence) around MEarth's later M dwarf targets. We describe a strategy with which MEarth can increase its expected planet yield by 2.5 × without new telescopes by shifting its sensitivity toward the smaller and cooler exoplanets that Kepler has demonstrated to be abundant.

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“…The observational procedure employed by HATNet to discover TEPs has been described in detail in several previous discovery papers (e.g., Bakos et al 2010;Latham et al 2009). In the following subsections we highlight specific details of this procedure that are pertinent to the discoveries of the four planets presented in this paper.…”

Section: Observationsmentioning

confidence: 99%

HAT-P-34b-HAT-P-37b: FOUR TRANSITING PLANETS MORE MASSIVE THAN JUPITER ORBITING MODERATELY BRIGHT STARS

Bakos

Hartman

Torres

et al. 2012

The Astronomical Journal

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We report the discovery of four transiting extrasolar planets (HAT-P-34b-HAT-P-37b) with masses ranging from 1.05 to 3.33 M J and periods from 1.33 to 5.45 days. These planets orbit relatively bright F and G dwarf stars (from V = 10.16 to V = 13.2). Of particular interest is HAT-P-34b which is moderately massive (3.33 M J ), has a high eccentricity of e = 0.441 ± 0.032 at a period of P = 5.452654 ± 0.000016 days, and shows hints of an outer component. The other three planets have properties that are typical of hot Jupiters.

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DISCOVERY OF A TRANSITING PLANET AND EIGHT ECLIPSING BINARIES IN HATNet FIELD G205

Cited by 92 publications

References 44 publications

On the formation of hot and warm Jupiters via secular high-eccentricity migration in stellar triples

On the formation of hot and warm Jupiters via secular high-eccentricity migration in stellar triples

Constraints on Planet Occurrence Around Nearby Mid-to-Late M Dwarfs From the Mearth Project

HAT-P-34b-HAT-P-37b: FOUR TRANSITING PLANETS MORE MASSIVE THAN JUPITER ORBITING MODERATELY BRIGHT STARS

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