The turbulent origin of spin–orbit misalignment in planetary systems

Fielding, Drummond B.; McKee, Christopher F.; Socrates, Aristostle; Cunningham, A. J.; Klein, Richard

doi:10.1093/mnras/stv836

Cited by 119 publications

(114 citation statements)

References 68 publications

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“…However, our earlier direct imaging survey finds no correlation between the orbital properties of the transiting planet and stellar multiplicity, suggesting that KozaiLidov migration is probably not the dominant channel for the generation of hot Jupiter spin-orbit misalignment. Instead, our results signal broad agreement with the primordial excitation of stellar obliquities (e.g., Lai 2014; Spalding & Batygin 2014Fielding et al 2015).…”

Section: Introductionsupporting

confidence: 71%

FRIENDS OF HOT JUPITERS. IV. STELLAR COMPANIONS BEYOND 50 au MIGHT FACILITATE GIANT PLANET FORMATION, BUT MOST ARE UNLIKELY TO CAUSE KOZAI–LIDOV MIGRATION

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Knutson

Hinkley

et al. 2016

ApJ

156

173

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Stellar companions can influence the formation and evolution of planetary systems, but there are currently few observational constraints on the properties of planet-hosting binary star systems. We search for stellar companions around 77 transiting hot Jupiter systems to explore the statistical properties of this population of companions as compared to field stars of similar spectral type. After correcting for survey incompleteness, we find that  47% 7% of hot Jupiter systems have stellar companions with semimajor axes between 50 and 2000 au. This is 2.9 times larger than the field star companion fraction in this separation range, with a significance of s 4.4 . In the 1-50 au range, only -+ 3.9 % 2.0 4.5 of hot Jupiters host stellar companions, compared to the field star value of  16.4% 0.7%, which is a s 2.7 difference. We find that the distribution of mass ratios for stellar companions to hot Jupiter systems peaks at small values and therefore differs from that of field star binaries which tend to be uniformly distributed across all mass ratios. We conclude that either wide separation stellar binaries are more favorable sites for gas giant planet formation at all separations, or that the presence of stellar companions preferentially causes the inward migration of gas giant planets that formed farther out in the disk via dynamical processes such as Kozai-Lidov oscillations. We determine that less than 20% of hot Jupiters have stellar companions capable of inducing KozaiLidov oscillations assuming initial semimajor axes between 1 and 5 au, implying that the enhanced companion occurrence is likely correlated with environments where gas giants can form efficiently.

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Section: Introductionsupporting

confidence: 71%

FRIENDS OF HOT JUPITERS. IV. STELLAR COMPANIONS BEYOND 50 au MIGHT FACILITATE GIANT PLANET FORMATION, BUT MOST ARE UNLIKELY TO CAUSE KOZAI–LIDOV MIGRATION

Ngo

Knutson

Hinkley

et al. 2016

ApJ

156

173

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“…Fielding et al (2015) found from their simulations of turbulent fragmentation typical spin-orbit angles Φ ∼ 40…”

Section: Discussionmentioning

confidence: 99%

Orbit Alignment in Triple Stars

Tokovinin

2017

ApJ

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Statistics of the angle Φ between orbital angular momenta in hierarchical triple systems with known inner visual or astrometric orbits are studied. Correlation between apparent revolution directions proves partial orbit alignment known from earlier works. The alignment is strong in triples with outer projected separation less than ∼50 AU, where the average Φ is about 20• . In contrast, outer orbits wider than 1000 AU are not aligned with the inner orbits. It is established that the orbit alignment decreases with increasing mass of the primary component. Average eccentricity of inner orbits in well-aligned triples is smaller than in randomly aligned ones. These findings highlight the role of dissipative interactions with gas in defining the orbital architecture of low-mass triple systems. On the other hand, chaotic dynamics apparently played a role in shaping more massive hierarchies. Analysis of projected configurations and triples with known inner and outer orbits indicates that the distribution of Φ is likely bimodal, where 80% of triples have Φ < 70• and the remaining ones are randomly aligned.

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“…Our evolution model takes into account the accretion history, which determines the protostellar size and nuclear state as well as the protostellar mass. The direction of angular momentum of the accreting material determines the outflow launching direction, as described in Fielding et al (2015). By construction, magnetic flux does not accrete onto sink particles.…”

Section: Methodsmentioning

confidence: 99%

“…We are not able to follow model M4P2.5l6 for the same evolutionary time due to the prohibitive computational expense. See Fielding et al (2015) for a more thorough resolution study of protostellar properties at different resolutions.…”

Section: A Resolution Studymentioning

confidence: 99%

Impact of Protostellar Outflows on Turbulence and Star Formation Efficiency in Magnetized Dense Cores

Offner

Chaban

2017

ApJ

110

126

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The star-forming efficiency of dense gas is thought to be set within cores by outflow and radiative feedback. We use magneto-hydrodynamic simulations to investigate the relation between protostellar outflow evolution, turbulence and star formation efficiency. We model the collapse and evolution of isolated dense cores for 0.5 Myr including the effects of turbulence, radiation transfer, and both radiation and outflow feedback from forming protostars. We show that outflows drive and maintain turbulence in the core environment even with strong initial fields. The star-formation efficiency decreases with increasing field strength, and the final efficiencies are 15 − 40%. The Stage 0 lifetime, during which the protostellar mass is less than the dense envelope, increases proportionally with the initial magnetic field strength and ranges from ∼ 0.1 − 0.4 Myr. The average accretion rate is well-represented by a tapered turbulent core model, which is a function of the final protostellar mass and is independent of the magnetic field strength. By tagging material launched in the outflow, we demonstrate that the outflow entrains about 3 times the actual launched gas mass, a ratio that remains roughly constant in time regardless of the initial magnetic field strength. However, turbulent driving increases for stronger fields since momentum is more efficiently imparted to non-outflow material. The protostellar outflow momentum is highest during the first 0.1 Myr and declines thereafter by a factor of 10 as the accretion rate diminishes.

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The turbulent origin of spin–orbit misalignment in planetary systems

Cited by 119 publications

References 68 publications

FRIENDS OF HOT JUPITERS. IV. STELLAR COMPANIONS BEYOND 50 au MIGHT FACILITATE GIANT PLANET FORMATION, BUT MOST ARE UNLIKELY TO CAUSE KOZAI–LIDOV MIGRATION

FRIENDS OF HOT JUPITERS. IV. STELLAR COMPANIONS BEYOND 50 au MIGHT FACILITATE GIANT PLANET FORMATION, BUT MOST ARE UNLIKELY TO CAUSE KOZAI–LIDOV MIGRATION

Orbit Alignment in Triple Stars

Impact of Protostellar Outflows on Turbulence and Star Formation Efficiency in Magnetized Dense Cores

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