The dynamical evolution of the Pleiades

@article{Converse2010TheDE,
  title={The dynamical evolution of the Pleiades},
  author={Joseph M. Converse and Steven William Stahler},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2010},
  volume={405},
  pages={666-680}
}
  • J. Converse, S. Stahler
  • Published 10 February 2010
  • Physics
  • Monthly Notices of the Royal Astronomical Society
We present the results of a numerical simulation of the history and future development of the Pleiades. This study builds on our previous one that established statistically the present-day structure of this system. Our simulation begins just after molecular cloud gas has been expelled by the embedded stars. We then follow, using an N-body code, the stellar dynamical evolution of the cluster to the present and beyond. Our initial state is that which evolves, over the 125 Myr age of the cluster… 

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References

SHOWING 1-10 OF 64 REFERENCES

The Distribution of Stellar Mass in the Pleiades

As part of an effort to understand the origin of open clusters, we present a statistical analysis of the currently observed Pleiades. Starting with a photometric catalog of the cluster, we employ a

The early expansion of cluster cores

The observed properties of young star clusters, such as the core radius and luminosity profile, change rapidly during the early evolution of the clusters. Here we present observations of six young

The formation of a bound star cluster: from the orion nebula cluster to the pleiades

Summary Direct N-body calculations are presented of the formation of Galactic clusters using GasEx, which is a variant of the code Nbody6. The calculations focus on the possible evolution of the

The formation and early dynamical evolution of bound stellar systems.

We present the results of numerical N-body calculations which simulate the dynamical evolution of young clusters as they emerge from molecular clouds. We follow the evolution of initially virialized

Gas expulsion and the destruction of massive young clusters

We examine the luminosity and dynamical mass estimates for young massive stellar clusters. For many young (<50 Myr) clusters, the luminosity and dynamical mass estimates differ by a significant

The Formation of Stellar Clusters in Turbulent Molecular Clouds: Effects of the Equation of State

We study the effect of varying the equation of state on the formation of stellar clusters in turbulent molecular clouds using three-dimensional, smoothed particle hydrodynamics simulations. Our

Formation of Massive Black Holes in Dense Star Clusters. I. Mass Segregation and Core Collapse

We study the early dynamical evolution of young dense star clusters by using Monte Carlo simulations for systems with up to N = 107 stars. Rapid mass segregation of massive main-sequence stars and

Star cluster ecology-IV. Dissection of an open star cluster: photometry

The evolution of star clusters is studied using N-body simulations in which the evolution of single stars and binaries is taken self-consistently into account. Initial conditions are chosen to

The Runaway Growth of Intermediate-Mass Black Holes in Dense Star Clusters

We study the growth rate of stars via stellar collisions in dense star clusters, calibrating our analytic calculations with direct N-body simulations of up to 65,536 stars, performed on the GRAPE

Cluster Formation in Contracting Molecular Clouds

We explore, through a simplified, semianalytic model, the formation of dense clusters containing massive stars. The parent cloud spawning the cluster is represented as an isothermal sphere. This
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