Super-Eccentric Migrating Jupiters

Socrates, Aristotle; Katz, Boaz; Dong, Subo; Tremaine, Scott

doi:10.1088/0004-637x/750/2/106

Cited by 114 publications

(141 citation statements)

References 17 publications

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“…The usual explanation for the occurrence of such eccentric orbits in short-period hot Jupiters is that they are moved in inwards by a process of "high-eccentricity migration," followed by circularization (e.g., Rasio & Ford 1996;Fabrycky & Tremaine 2007;Naoz et al 2011;Socrates et al 2012a).…”

Section: A Massive Planet In An Eccentric Orbitmentioning

confidence: 99%

“…The circularization timescale can be estimated from ( The value of the quality factor, Q P , is unclear, but if we take it as 10 5 (e.g., Socrates et al 2012b), then we obtain for WASP-89b a circularization timescale of ∼2 Gyr. Here, the large mass of the planet prevents circularization in less than 1 Gyr despite the short orbit.…”

Section: A Massive Planet In An Eccentric Orbitmentioning

confidence: 99%

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THREE WASP-SOUTH TRANSITING EXOPLANETS: WASP-74b, WASP-83b, AND WASP-89b

Hellier

Anderson

Cameron

et al. 2015

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We report the discovery of three new transiting hot Jupiters by WASP-South together with the TRAPPIST photometer and the Euler/CORALIE spectrograph. WASP-74b orbits a star of V = 9.7, making it one of the brighter systems accessible to southern telescopes. It is a 0.95M Jup planet with a moderately bloated radius of 1.5 R Jup in a 2 day orbit around a slightly evolved F9 star. WASP-83b is a Saturn-mass planet at 0.3 M Jup with a radius of 1.0 R Jup . It is in a 5 day orbit around a fainter (V = 12.9) G8 star. WASP-89b is a 6 M Jup planet in a 3 day orbit with an eccentricity of e = 0.2. It is thus similar to massive, eccentric planets such as XO-3b and HAT-P-2b, except that those planets orbit F stars whereas WASP-89 is a K star. The V = 13.1 host star is magnetically active, showing a rotation period of 20.2 days, while star spots are visible in the transits. There are indications that the planet's orbit is aligned with the stellar spin. WASP-89 is a good target for an extensive study of transits of star spots.

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Section: A Massive Planet In An Eccentric Orbitmentioning

confidence: 99%

Section: A Massive Planet In An Eccentric Orbitmentioning

confidence: 99%

THREE WASP-SOUTH TRANSITING EXOPLANETS: WASP-74b, WASP-83b, AND WASP-89b

Hellier

Anderson

Cameron

et al. 2015

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“…Indeed, three-body encounters more often than not disrupt VLM multiples (Moeckel & Bate 2010). A more intriguing mechanism for SDSS J0006−0852AB is Kozai-Lidov eccentricity perturbations induced by LP 704-48, followed by circularization through tidal friction (KCTF; Kozai 1962;Harrington 1968;Kiseleva et al 1998;Fabrycky & Tremaine 2007;Socrates et al 2012). …”

Section: On the Formation Of Lp 704-48/sdss J0006−0852abmentioning

confidence: 99%

Discovery of a Very Low Mass Triple With Late-M and T Dwarf Components: Lp 704-48/SDSS J0006–0852ab

Burgasser

Luk

Dhital

et al. 2012

ApJ

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We report the identification of the M9 dwarf SDSS J000649.16−085246.3 as a spectral binary and radial velocity (RV) variable with components straddling the hydrogen-burning mass limit. Low-resolution near-infrared spectroscopy reveals spectral features indicative of a T dwarf companion, and spectral template fitting yields component types of M8.5 ± 0.5 and T5 ± 1. High-resolution near-infrared spectroscopy with Keck/NIRSPEC reveals pronounced RV variations with a semi-amplitude of 8.2 ± 0.4 km s −1 . From these we determine an orbital period of 147.6 ± 1.5 days and eccentricity of 0.10 ± 0.07, making SDSS J0006−0852AB the third tightest very low mass binary known. This system is also found to have a common proper motion companion, the inactive M7 dwarf LP 704-48, at a projected separation of 820 ± 120 AU. The lack of Hα emission in both M dwarf components indicates that this system is relatively old, as confirmed by evolutionary model analysis of the tight binary. LP 704-48/SDSS J0006−0852AB is the lowest-mass confirmed triple identified to date, and one of only seven candidate and confirmed triples with total masses below 0.3 M currently known. We show that current star and brown dwarf formation models cannot produce triple systems like LP 704-48/SDSS J0006−0852AB, and we rule out Kozai-Lidov perturbations and tidal circularization as a viable mechanism to shrink the inner orbit. The similarities between this system and the recently uncovered low-mass eclipsing triples NLTT 41135AB/41136 and LHS 6343ABC suggest that substellar tertiaries may be common in wide M dwarf pairs.

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“…Other ideas have been put forward (e.g. Triaud et al 2010;Morton & Johnson 2011;Socrates et al 2012), which include more "violent" migration mechanisms. Discoveries of giant planets on wide orbits of tens to hundreds AU (Marois et al 2008;Lagrange et al 2010) also raise questions.…”

Section: Introductionmentioning

confidence: 99%

The frequency of giant planets around metal-poor stars

Mortier

Santos

Sozzetti

et al. 2012

A&A

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Context. The discovery of about 700 extrasolar planets, so far, has lead to the first statistics concerning extrasolar planets. The presence of giant planets seems to depend on stellar metallicity and mass. For example, they are more frequent around metal-rich stars, with an exponential increase in planet occurrence rates with metallicity. Aims. We analyzed two samples of metal-poor stars (−2.0 ≤ [Fe/H] ≤ 0.0) to see if giant planets are indeed rare around these objects. Radial velocity datasets were obtained with two different spectrographs (HARPS and HIRES). Detection limits for these data, expressed in minimum planetary mass and period, are calculated. These produce trustworthy numbers for the planet frequency. Methods. A general Lomb-Scargle (GLS) periodogram analysis was used together with a bootstrapping method to produce the detection limits. Planet frequencies were calculated based on a binomial distribution function within metallicity bins. Results. Almost all hot Jupiters and most giant planets should have been found in these data. Hot Jupiters around metal-poor stars have a frequency lower than 1.0% at one sigma. Giant planets with periods up to 1800 days, however, have a higher frequency of f p = 2.63 +2.5 −0.8 %. Taking into account the different metallicities of the stars, we show that giant planets appear to be very frequent ( f p = 4.48 +4.04 −1.38 %) around stars with [Fe/H] > −0.7, while they are rare around stars with [Fe/H] ≤ −0.7 (≤2.36% at one sigma). Conclusions. Giant planet frequency is indeed a strong function of metallicity, even in the low-metallicity tail. However, the frequencies are most likely higher than previously thought.

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Super-Eccentric Migrating Jupiters

Cited by 114 publications

References 17 publications

THREE WASP-SOUTH TRANSITING EXOPLANETS: WASP-74b, WASP-83b, AND WASP-89b

THREE WASP-SOUTH TRANSITING EXOPLANETS: WASP-74b, WASP-83b, AND WASP-89b

Discovery of a Very Low Mass Triple With Late-M and T Dwarf Components: Lp 704-48/SDSS J0006–0852ab

The frequency of giant planets around metal-poor stars

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