The Stability and Fates of Hierarchical Two-Planet Systems

Petrovich, Cristóbal

doi:10.1088/0004-637x/808/2/120

Cited by 105 publications

(100 citation statements)

References 55 publications

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“…On the other hand, only -+ 3.9 % 2.0 4.5 of hot Jupiters have stellar companions with separations between 1 and 50 au, while  16.4% 0.7% of field stars have stellar companions in this range, corresponding to a s 2.7 difference. We choose a lower limit of 1 au to avoid systems where the stellar companion could eject the hot Jupiter (Mardling & Aarseth 2001;Petrovich 2015b). We note that if we relax this lower limit and considered all companions with separations less than 50 au, we find that hot Jupiter hosts have a companion fraction of -+ 3.9 % 2.0 4.6 while field stars have a companion fraction of  22% 1%, which is a difference of s 3.8 .…”

Section: Stellar Companion Fraction For Hot Jupiter Hosts Versus Fielmentioning

confidence: 99%

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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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.

show abstract

Section: Stellar Companion Fraction For Hot Jupiter Hosts Versus Fielmentioning

confidence: 99%

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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show abstract

“…1/3 and a in (a out ) is the semimajor axis of the inner (outer) planet (Chambers et al 1996;Yoshinaga et al 1999;Fang & Margot 2013;Pu & Wu 2015;Petrovich 2015). When all planets have e = 0.03 (e = 0.10), the maximum number of stable Earth-mass planets within 0.4-1 AU is 7-8 (4-5).…”

Section: Frequency Of Earth-mass Planets At 025-2 Au Around Solar-tymentioning

confidence: 99%

Rocky Planet Formation: Quick and Neat

Kenyon

Najita

Bromley

2016

ApJ

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We reconsider the commonly held assumption that warm debris disks are tracers of terrestrial planet formation. The high occurrence rate inferred for Earthmass planets around mature solar-type stars based on exoplanet surveys (∼ 20%) stands in stark contrast to the low incidence rate (≤ 2%-3%) of warm dusty debris around solar-type stars during the expected epoch of terrestrial planet assembly (∼ 10 Myr). If Earth-mass planets at AU distances are a common outcome of the planet formation process, this discrepancy suggests that rocky planet formation occurs more quickly and/or is much neater than traditionally believed, leaving behind little in the way of a dust signature. Alternatively, the incidence rate of terrestrial planets has been overestimated or some previously unrecognized physical mechanism removes warm dust efficiently from the terrestrial planet region. A promising removal mechanism is gas drag in a residual gaseous disk with a surface density 10 −5 of the minimum mass solar nebula.

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“…This distinction is only significant for the very massive planets we consider here. Recently, Petrovich (2015) has also explored the role of high eccentricity in modifying the stability boundary.…”

Section: Previous Workmentioning

confidence: 99%

Orbital Stability of Multi-Planet Systems: Behavior at High Masses

Morrison

Kratter

2016

ApJ

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In the coming years, high-contrast imaging surveys are expected to reveal the characteristics of the population of wide-orbit, massive, exoplanets. To date, a handful of wide planetary mass companions are known, but only one such multi-planet system has been discovered: HR 8799. For low mass planetary systems, multi-planet interactions play an important role in setting system architecture. In this paper, we explore the stability of these high mass, multi-planet systems. While empirical relationships exist that predict how system stability scales with planet spacing at low masses, we show that extrapolating to super-Jupiter masses can lead to up to an order of magnitude overestimate of stability for massive, tightly packed systems. We show that at both low and high planet masses, overlapping mean-motion resonances trigger chaotic orbital evolution, which leads to system instability. We attribute some of the difference in behavior as a function of mass to the increasing importance of second order resonances at high planet-star mass ratios. We use our tailored high mass planet results to estimate the maximum number of planets that might reside in double component debris disk systems, whose gaps may indicate the presence of massive bodies.

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The Stability and Fates of Hierarchical Two-Planet Systems

Cited by 105 publications

References 55 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

Rocky Planet Formation: Quick and Neat

Orbital Stability of Multi-Planet Systems: Behavior at High Masses

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