The Occurrence and Architecture of Exoplanetary Systems

Winn, Joshua N.; Fabrycky, Daniel C.

doi:10.1146/annurev-astro-082214-122246

Cited by 837 publications

(748 citation statements)

References 294 publications

(314 reference statements)

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“…In this paper we show how this absence of planets may be a natural consequence of close binary formation, formalising an explanation that was briefly proposed by Welsh et al (2014a), Armstrong et al (2014), Martin & Triaud (2014) and Winn & Fabrycky (2014). A popular theory proposes that most very close binaries ( 7 d) are initially formed at wider separations.…”

Section: Introductionsupporting

confidence: 77%

No circumbinary planets transiting the tightestKeplerbinaries – a possible fingerprint of a third star

Martin

Mazeh

Fabrycky

2015

Mon. Not. R. Astron. Soc.

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The Kepler mission has yielded the discovery of eight circumbinary systems, all found around eclipsing binaries with periods greater than 7 d. This is longer than the typical eclipsing binary period found by Kepler, and hence there is a dearth of planets around the closest binaries. In this paper we suggest how this dearth may be explained by the presence of a distant stellar tertiary companion, which shrunk the inner binary orbit by the process of Kozai cycles and tidal friction, a mechanism that has been implicated for producing most binaries with periods below 7 d. We show that the geometry and orbital dynamics of these evolving triple-star systems are highly restrictive for a circumbinary planet, which is subject itself to Kozai modulation, on one hand, and can shield the two inner stars from their Kozai cycle and subsequent shrinking, on the other hand. Only small planets on wide and inclined orbits may form, survive and allow for the inner binary shrinkage. Those are difficult to detect.

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Section: Introductionsupporting

confidence: 77%

No circumbinary planets transiting the tightestKeplerbinaries – a possible fingerprint of a third star

Martin

Mazeh

Fabrycky

2015

Mon. Not. R. Astron. Soc.

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“…On the other hand, results from the Stardust mission showed that comet dust contains minerals formed at high temperature, presumably near to the Sun (Brownlee et al 2006). Meanwhile, many extrasolar systems with gas giant planets close to their stars have been discovered, presenting a challenge to formation models (e.g., Mayor and Queloz 1995;Winn and Fabrycky 2015). Finally, recent observations have uncovered evidence of ice in unexpected places in the inner Solar System, including the population of 'Main-Belt Comets' (MBCs) which have stable asteroidlike orbits, inside the snow line, but which demonstrate comet-like activity (Hsieh and Jewitt 2006).…”

Section: Introductionmentioning

confidence: 99%

The Main Belt Comets and ice in the Solar System

Snodgrass

Agarwal

Combi

et al. 2017

Astron Astrophys Rev

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We review the evidence for buried ice in the asteroid belt; specifically the questions around the so-called Main Belt Comets (MBCs). We summarise the evidence for water throughout the Solar System, and describe the various methods for detecting it, including remote sensing from ultraviolet to radio wavelengths. We review progress in the first decade of study of MBCs, including observations, modelling of ice survival, and discussion on their origins. We then look at which methods will likely be most effective for further progress, including the key challenge of direct detection of (escaping) water in these bodies.

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“…Wu & Lithwick 2011;Naoz et al 2011;Petrovich 2015;Anderson et al 2015) as well as in explaining their preferentially circular orbits compared with planets that orbit more distantly, which have a wide range of eccentricities (e.g. Rasio et al 1996;Winn & Fabrycky 2015). The mechanisms responsible for tidal dissipation are not fully understood, though much progress has been made over the past decade (Ogilvie & Lin 2004;Wu 2005;Ivanov & Papaloizou 2007;Ogilvie & Lin 2007;Goodman & Lackner 2009;Remus et al 2012;Favier et al 2014;Ogilvie 2014).…”

Section: Introductionmentioning

confidence: 99%

Non-linear tides in a homogeneous rotating planet or star: global modes and elliptical instability

Barker

Braviner

Ogilvie

2016

Mon. Not. R. Astron. Soc.

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We revisit the global modes and instabilities of homogeneous rotating ellipsoidal fluid masses, which are the simplest global models of rotationally and tidally deformed gaseous planets or stars. The tidal flow in a short-period planet may be unstable to the elliptical instability, a hydrodynamic instability that can drive tidal evolution. We perform a global (and local WKB) analysis to study this instability using the elegant formalism of Lebovitz & Lifschitz. We survey the parameter space of global instabilities with harmonic orders 5, for planets with spins that are purely aligned (prograde) or anti-aligned (retrograde) with their orbits. In general, the instability has a much larger growth rate if the planetary spin and orbit are anti-aligned rather than aligned. We have identified a violent instability for anti-aligned spins outside of the usual frequency range for the elliptical instability (when n Ω −1, where n and Ω are the orbital and spin angular frequencies, respectively) if the tidal amplitude is sufficiently large. We also explore the instability in a rigid ellipsoidal container, which is found to be quantitatively similar to that with a realistic free surface. Finally, we study the effect of rotation and tidal deformation on mode frequencies. We find that larger rotation rates and larger tidal deformations both decrease the frequencies of the prograde sectoral surface gravity modes. This increases the prospect of their tidal excitation, potentially enhancing the tidal response over expectations from linear theory. In a companion paper, we use our results to interpret global simulations of the elliptical instability.

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The Occurrence and Architecture of Exoplanetary Systems

Cited by 837 publications

References 294 publications

No circumbinary planets transiting the tightestKeplerbinaries – a possible fingerprint of a third star

No circumbinary planets transiting the tightestKeplerbinaries – a possible fingerprint of a third star

The Main Belt Comets and ice in the Solar System

Non-linear tides in a homogeneous rotating planet or star: global modes and elliptical instability

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