Cross-sections for planetary systems interacting with passing stars and binaries

Li, Gongjie; Adams, Fred C.

doi:10.1093/mnras/stv012

Cited by 93 publications

(140 citation statements)

References 63 publications

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“…The giant-planet orbits are vulnerable to changes during scattering encounters, and the cross sections for their disruption have been calculated previously (Adams & Laughlin 2001;Li & Adams 2015). Specifically, the cross section for doubling the eccentricity of Neptune, or the spread in inclination angles, is σ dis ≈ (400 au) 2 .…”

Section: −1mentioning

confidence: 96%

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Interaction Cross Sections and Survival Rates for Proposed Solar System Member Planet Nine

Adams

2016

ApJL

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Motivated by the report of a possible new planetary member of the solar system, this work calculates cross sections for interactions between passing stars and this proposed Planet Nine. Evidence for the new planet is provided by the orbital alignment of Kuiper belt objects, and other solar system properties, which suggest a Neptune-mass object on an eccentric orbit with a semimajor axis a 9 ≈ 400-1500 au. With such a wide orbit, Planet Nine has a large interaction cross section and is susceptible to disruption by passing stars. Using a large ensemble of numerical simulations (several million) and Monte Carlo sampling, we calculate the cross sections for different classes of orbit-altering events: (A) scattering the planet into its proposed orbit from a smaller orbit, (B) ejecting it from the solar system from its current orbit, (C) capturing the planet from another system, and (D) capturing a free-floating planet. Results are presented for a range of orbital elements with planetary mass m 9 = 10 M ⊕ . Removing Planet Nine from the solar system is the most likely outcome. Specifically, we obtain ejection cross sections s int ∼ 5 × 10 6 au 2 (5 × 10 4 au 2 ) for environments corresponding to the birth cluster (field). With these cross sections, Planet Nine is likely to be ejected if the Sun resides within its birth cluster longer than Δt  100 Myr. The probability of ejecting Planet Nine due to passing field stars is 3% over the age of the Sun. Probabilities for producing the inferred Planet Nine orbit are low (5%).

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Section: −1mentioning

confidence: 96%

“…In order to calculate the cross sections for interactions between the solar system and passing stars, we perform a large ensemble of numerical experiments using previously developed techniques (for details, see Adams & Laughlin 2001;Li & Adams 2015). This approach is summarized below.…”

Section: Interaction Cross Sectionsmentioning

confidence: 99%

Interaction Cross Sections and Survival Rates for Proposed Solar System Member Planet Nine

Adams

2016

ApJL

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“…The importance of passing stars in perturbing planetary bodies should increase with stellar density, the cross sections of planetary systems, and the lifetimes of planetary systems inside star clusters. Laughlin & Adams (1998), Spurzem & Lin (2003), Adams & Laughlin (2001 and Li & Adams (2015) have shown via scattering experiments that the orbits of planetary systems in star clusters must be changed during encounters with passing stars.…”

Section: Introductionmentioning

confidence: 99%

“…It is important to simulate multiplanet systems both because they exist and because planet-planet interactions may be as important as stellar encounters in modifying orbits (Hurley et al 2008, p. 137;Malmberg et al 2011, Boley et al 2012. A significant advance was recently made by Hao et al (2013) and by Li & Adams (2015), who used Monte Carlo scattering experiments to conclusively demonstrate that flybys strongly affect the evolution of multiplanet systems in dense open clusters.…”

Section: Introductionmentioning

confidence: 99%

Dynamical Interactions Make Hot Jupiters in Open Star Clusters

Shara

Hurley

Mardling

2016

ApJ

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Explaining the origin and evolution of exoplanetary hot Jupiters remains a significant challenge. One possible mechanism for the production of hot Jupitersis planet-planet interactions, which produce them from planets born far from their host stars but near their dynamical stability limits. In the much more likely case of planets born far from their dynamical stability limits, can hot Jupiters be formed in star clusters? Our N-body simulations answer this question in the affirmative, and show that hot Jupiter formation is not a rare event, occurring in ∼1% of star cluster planetary systems. We detail three case studies of the dynamics-induced births of hot Jupiters on highly eccentric orbits that can only occur inside star clusters. The hot Jupiters' orbits bear remarkable similarities to those of some of the most extreme exoplanets known: HAT-P-32b, HAT-P-2b, HD 80606b, and GJ 876d. If stellar perturbations formed these hot Jupiters, then our simulations predict that these very hot inner planets are often accompanied by much more distant gas giants in highly eccentric orbits.

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“…Orbital parameters of the two planets orbiting Pr0211 in M44 (Malavolta et al 2016) et al. 2013;Li & Adams 2015). The necessarily very high stellar density means the influence of the environment is much stronger and disc destruction more likely than for the short-lived clusters ).…”

Section: Introductionmentioning

confidence: 99%

Did a stellar fly-by shape the planetary system around Pr 0211 in the cluster M44?

Pfalzner¹,

Bhandare²,

Vincke³

2018

A&A

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Aims. Out of the ∼ 3000 exoplanets detected so far, only fourteen planets are members of open clusters: among them an exoplanet system around Pr 0211 in the cluster M44 which consists of at least two planets with the outer planet moving on a highly eccentric orbit at 5.5 AU. One hypothesis is that a close fly-by of a neighbouring star was responsible for the eccentric orbit. We test this hypothesis. Methods. First we determine the type of fly-by that would lead to the observed parameters and then use this result to determine the history of such fly-bys in simulations of the early dynamics in an M44-like environment. Results. We find that although very close fly-bys are required to obtain the observed properties of Pr 0211c, such fly-bys are relatively common due to the high stellar density and longevity of the cluster. About 10% of stars actually experience a fly-by that would lead to such a small system-size as observed for Pr0211 or even smaller. Such close fly-bys are most frequent during the first 1-2 Myr after cluster formation, corresponding to a cluster age ≤ 3 Myr. It is unclear whether planets generally form on such short timescales. However, afterwards the close fly-by rate is still 0.2-0.5 Myr −1 , which means extrapolating this to the age of M44 12%-20% of stars would experience such close fly-bys over this timespan. Conclusions. Our simulations show that the fly-by scenario is a realistic option for the formation of eccentricity orbits of the planets in M44. The occurance of such events is relatively high leading to the expectation that similar systems are likely common in open clusters in general.

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Cross-sections for planetary systems interacting with passing stars and binaries

Cited by 93 publications

References 63 publications

Interaction Cross Sections and Survival Rates for Proposed Solar System Member Planet Nine

Interaction Cross Sections and Survival Rates for Proposed Solar System Member Planet Nine

Dynamical Interactions Make Hot Jupiters in Open Star Clusters

Did a stellar fly-by shape the planetary system around Pr 0211 in the cluster M44?

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