The dynamical fate of planetary systems in young star clusters

Zheng, Xiaochen; Kouwenhoven, M. B. N.; Wang, Long

doi:10.1093/mnras/stv1832

Cited by 52 publications

(48 citation statements)

References 110 publications

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“…Once the intra-cluster gas is gone, the cluster becomes supervivial temporarily, and the subsequent reestablishment of virial equilibrium may lead to a temporary surge of planet ejection rates. In a recent study, Zheng et al (2015) carry out direct N -body simulations of clusters with different initial morphologies and initial virial states. They conclude that non-equilibrium conditions in host clusters can indeed boost the ejection rate, and that for a cluster of N = 1000 stars, a virial equilibrium is reestablished at an energy equalpartition timescale of 5 Myr, after which the ejection rates becomes steady again.…”

Section: Enhanced Planet Ejection Efficiency Due To the Structural Evmentioning

confidence: 99%

On the survivability of planets in young massive clusters and its implication of planet orbital architectures in globular clusters

Cai

Zwart

Kouwenhoven

et al. 2019

Monthly Notices of the Royal Astronomical Society

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As of August 2019, among the more than 4000 confirmed exoplanets, only one has been detected in a globular cluster (GC) M4. The scarce of exoplanet detections motivates us to employ direct N -body simulations to investigate the dynamical stability of planets in young massive clusters (YMCs), which are potentially the progenitors of GCs. In an N = 128k cluster of virial radius 1.7 pc (comparable to Westerlund-1), our simulations show that most wide-orbit planets (a ≥ 20 au) will be ejected within a timescale of 10 Myr. Interestingly, more than 70% of planets with a < 5 au survive in the 100 Myr simulations. Ignoring planet-planet scattering and tidal damping, the survivability at t Myr as a function of initial semi-major axis a 0 in au in such a YMC can be described as f surv (a 0 , t) = −0.33 log 10 (a 0 ) 1 − e −0.0482t + 1. Upon ejection, about 28.8% of free-floating planets (FFPs) have sufficient speeds to escape from the host cluster at a crossing timescale. The other FFPs will remain bound to the cluster potential, but the subsequent dynamical evolution of the stellar system can result in the delayed ejection of FFPs from the host cluster. Although a full investigation of planet population in GCs requires extending the simulations to multi-Gyr, our results suggest that wideorbit planets and free-floating planets are unlikely to be found in GCs.

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Section: Enhanced Planet Ejection Efficiency Due To the Structural Evmentioning

confidence: 99%

On the survivability of planets in young massive clusters and its implication of planet orbital architectures in globular clusters

Cai

Zwart

Kouwenhoven

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Dynamical interactions with a distant companion may increase turbulent velocities in the protoplanetary disk, thereby preventing materials from condensing (Mayer et al 2005). By searching for stellar companions to known planetary systems we can constrain their potential effects on these planetary systems, albeit with the caveat that close encounters between stars forming in crowded cluster environments may have similar effects (e.g., Bonnell et al 2001;Spurzem et al 2009;Hao et al 2013;Zheng et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Friends of Hot Jupiters. Iii. An Infrared Spectroscopic Search for Low-Mass Stellar Companions

Piskorz

Knutson

Ngo

et al. 2015

ApJ

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Surveys of nearby field stars indicate that stellar binaries are common, yet little is known about the effects that these companions may have on planet formation and evolution. The Friends of Hot Jupiters project uses three complementary techniques to search for stellar companions to known planet-hosting stars: radial velocity monitoring, adaptive optics imaging, and near-infrared spectroscopy. In this paper, we examine high-resolution K band infrared spectra of fifty stars hosting gas giant planets on short-period orbits. We use spectral fitting to search for blended lines due to the presence of cool stellar companions in the spectra of our target stars, where we are sensitive to companions with temperatures between 3500 and 5000 K and projected separations less than 100 AU in most systems. We identify eight systems with candidate low-mass companions, including one companion that was independently detected in our AO imaging survey. For systems with radial velocity accelerations, a spectroscopic non-detection rules out scenarios involving a stellar companion in a high inclination orbit. We use these data to place an upper limit on the stellar binary fraction at small projected separations, and show that the observed population of candidate companions is consistent with that of field stars and also with the population of wide-separation companions detected in our previous AO survey. We find no evidence that spectroscopic stellar companions are preferentially located in systems with short-period gas giant planets on eccentric and/or misaligned orbits.

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“…Therefore the concept of a hard-soft boundary as discussed above does not apply. However, N-body models do predict that the distribution of planet semi-major axes (or periods) should also be truncated by dynamical encounters [99], though here it is the encounter rate that sets the limit rather than the encounter energy.…”

Section: Changes To the Companion Frequencymentioning

confidence: 99%

“…Dynamical Processing of Stars and Planets Through Star Clusters Aaron M. Geller period) distribution for planets should be truncated by encounters (as also discussed above, [99]) and that eccentricities are most easily modified in planets with wider orbits [90].…”

Section: Pos(bash2015)006mentioning

confidence: 99%

Dynamical Processing of Stars and Planets Through Star Clusters

Geller¹

2016

Proceedings of Frank N. Bash Symposium 2015 — PoS(BASH2015)

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Most stars are born in clustered environments that are far denser than the Solar Neighborhood.Yet, star clusters can be hostile locations, where close stellar encounters can be frequent and can have violent consequences, including direct stellar collisions. Such encounters can dramatically alter stellar and planetary systems, and can produce exotic stars that define new pathways in stellar evolution. Understanding how, and to what extent, such "dynamically processing" occurs in star clusters may be critical for our understanding of the architectures of today's observed stellar and planetary systems, as well as the origins of X-ray sources, blue stragglers, sub-subgiants, and other stellar exotica. In this contribution, I discuss the impacts of living in a star cluster on its inhabitants, through a review of observational and theoretical efforts to study these complex systems. Throughout, I assert that binary stars are intimately linked to both the dynamical evolution of star clusters and the effects that stellar encounters within these environments have on their stellar and planetary populations. I conclude that in order to properly interpret our present and future observations of stars and planets, both in star clusters and the field, and particularly if we attempt to use these observations to inform star and planet formation theory, we must first account for the imprint left by stellar encounters within a clustered birth environment.

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The dynamical fate of planetary systems in young star clusters

Cited by 52 publications

References 110 publications

On the survivability of planets in young massive clusters and its implication of planet orbital architectures in globular clusters

On the survivability of planets in young massive clusters and its implication of planet orbital architectures in globular clusters

Friends of Hot Jupiters. Iii. An Infrared Spectroscopic Search for Low-Mass Stellar Companions

Dynamical Processing of Stars and Planets Through Star Clusters

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