Dynamics of Planetary Systems in Star Clusters

  title={Dynamics of Planetary Systems in Star Clusters},
  author={Rainer Spurzem and Mirek Giersz and Douglas C Heggie and Douglas N. C. Lin},
  journal={The Astrophysical Journal},
At least 10%-15% of nearby Sunlike stars have known Jupiter-mass planets. In contrast, very few planets are found in mature open and globular clusters such as the Hyades and 47 Tuc. We explore here the possibility that this dichotomy is due to the postformation disruption of planetary systems associated with the stellar encounters in long-lived clusters. One supporting piece of evidence for this scenario is the discovery of freely floating low-mass objects in star forming regions. We use two… 
The dynamical evolution of multiplanet systems in open clusters
The majority of stars form in star clusters and many are thought to have planetary companions. We demonstrate that multi-planet systems are prone to instabilities as a result of frequent stellar
Close encounters involving free-floating planets in star clusters
Instabilities in planetary systems can result in the ejection of planets from their host system, resulting in free-floating planets (FFPs). If this occurs in a star cluster, the FFP may remain bound
The effects of dynamical interactions on planets in young substructured star clusters
We present N-body simulations of young substructured star clusters undergoing various dynamical evolutionary scenarios and examine the direct effects of interactions in the cluster on planetary
Probing the Survival of Planetary Systems in Globular Clusters with Tidal Disruption Events
Among the growing list of confirmed exoplanets, the number of planets identified in dense star clusters remains sparse. Previous analyses have suggested this may be due in part to dynamical
Planetary systems in a star cluster I: the Solar system scenario
Young stars are mostly found in dense stellar environments, and even our own Solar system may have formed in a star cluster. Here, we numerically explore the evolution of planetary systems similar to
How Do Disks and Planetary Systems in High-mass Open Clusters Differ from Those around Field Stars?
Only star clusters that are sufficiently compact and massive survive largely unharmed beyond 10 Myr. However, their compactness means a high stellar density which can lead to strong gravitational
Fly-by encounters between two planetary systems I: Solar system analogues
Stars formed in clusters can encounter other stars at close distances. In typical open clusters in the Solar neighbourhood containing hundreds or thousands of member stars, 10–20 per cent of
Stability of multiplanetary systems in star clusters
Most stars form in star clusters and stellar associations. However, only about ˜1 per cent of the presently known exoplanets are found in these environments. To understand the roles of star cluster
Detectability of Free Floating Planets in Open Clusters with the James Webb Space Telescope
Recent observations have shown the presence of extra-solar planets in Galactic open stellar clusters, such as in Praesepe (M44). These systems provide a favorable environment for planetary formation
Can habitable planets form in clustered environments
We present observational evidence of environmental effects on the formation and evolution of planetary systems. We combine catalogues of resolved protoplanetary discs (PPDs) and young stellar objects


The Modification of Planetary Orbits in Dense Open Clusters
We show that Jovian planets will frequently experience orbital disruption due to interactions with binary stars in their birth clusters. We attack the problem using a Monte Carlo approach and
We find that free-floating planets can remain bound to an open cluster for much longer than was previously calculated: of the order of the cluster half-mass relaxation timescale as opposed to the
Free‐floating planets in stellar clusters?
We have simulated encounters between planetary systems and single stars in various clustered environments. This allows us to estimate the fraction of systems liberated, the velocity distribution of
Dynamical Instabilities and the Formation of Extrasolar Planetary Systems
The existence of a dominant massive planet, Jupiter, in our solar system, although perhaps essential for long-term dynamical stability and the development of life, may not be typical of planetary
Free-Floating Planets: Not So Surprising
We find that free-floating planets can remain bound to a star cluster for much longer than was previously assumed: of the order of the cluster half-mass relaxation timescale as opposed to the
On the Origin of Massive Eccentric Planets
We propose a merger scenario for the newly discovered extrasolar planets around 70 Vir (Marcy & Butler) and HD 114762 (Latham, Stefanik, & Mazeh; Marcy & Butler). These planets have mass Mp sin i =
Spin-orbit evolution of short-period planets
The negligible eccentricity of all extrasolar planets with periods less than 6 days can be accounted for by dissipation of tidal disturbances within their envelopes that are induced by their host
Dynamical Origin of Extrasolar Planet Eccentricity Distribution
We explore the possibility that the observed eccentricity distribution of extrasolar planets arose through planet-planet interactions, after the initial stage of planet formation was complete. Our
Orbital migration of the planetary companion of 51 Pegasi to its present location
THE recent discovery1 and confirmation2 of a possible planetary companion orbiting the solar-type star 51 Pegasi represent a breakthrough in the search for extrasolar planetary systems. Analysis of
Predictions for the frequency and orbital radii of massive extrasolar planets
We investigate the migration of massive extrasolar planets caused by gravitational interaction with a viscous protoplanetary disc. We show that a model in which planets form at 5 au at a constant