[PDF] Top 20 The Formation and Dynamical Evolution of Young Star Clusters

... the clusters tend to be supervirial, and some stars escape right away ( see the virial ratio given in Table 2 ) ...leaky clusters and OB ...leaky clusters and as associations in Portegies Zwart et ... See full document

... the evolution of 2000 mass-less particles placed on orbits librating around Neptune’s L4 and L5 Lagrange points (1000 bodies each) in a planetary system with the four giant planets (Jupiter, Saturn, Uranus and ... See full document

... the dynamical (and chemical) evolution of star clusters (Kouwenhoven et ...lower star cluster could still host stars sufficiently massive to experience a supernova or even a Wolf- Rayet ... See full document

... of young clusters with N-body simulations of clusters including the effects of rapid gas loss, we argue that young clusters are not in Virial ...the clusters and not related to ... See full document

... dwarf formation proposes that protostellar discs can fragment into objects with masses above a few Jupiter masses at large semimajor ...parent star-forming ...subsequent dynamical evolution ... See full document

... that clusters with more high-mass stars lose relatively more mass through stellar evolution, but the response to this mass-loss is to expand and hence significantly slow their dynamical ...have ... See full document

... The dynamical evolution of planetary systems, after the evaporation of the accretion disk, is the result of the competition between tidal dissipation and the net an- gular momentum loss of the ...tidal ... See full document

... the dynamical state of the stars is crucial to how they react to gas expulsion, slow-moving stars will ‘feel’ the effects of gas expulsion far less than fast-moving stars (relative to their equilibrium ...of ... See full document

... the formation and evolution of young star clusters using SPH and direct N -body ...local star-formation efficiency that depends on the local gas ...known star forming ... See full document

... massive star clusters are the progenitors of globular clusters, their mass function must evolve with time to resemble the globular cluster mass function through mass loss within a cluster or the ... See full document

... from clusters in which the stars and gas are both dynamically relaxed and in global virial equilibrium (but see Lada et ...global star formation efficiency (SFE) in the ...exact dynamical ... See full document

... and evolution of galaxies is one of the most active research fields in ...galaxy formation and evolution is modeled by the Λ CDM, which stands for Cold Dark Mat- ter with dark energy field identified ... See full document

... experience copious mass loss in the Wolf-Rayet phase fol- lowed by a supernova explosion. Such evolution may en- rich most of the disk in the cluster by r-processed elements (Portegies Zwart et al. 2018a). The ... See full document

... the star-to-BD ratio ( uncertainties in distances, ages, use of different evolutionary models, reddening laws, membership issues, small sample sizes; see, ...nearby star- forming regions, theoretical ... See full document

... nearby clusters already covered by the UKIDSS ...distant clusters, as it is both more sensitive than the GCS, and covers a wider area of ...detect young brown dwarfs in associations covered by both ... See full document

... to star-forming regions, and might therefore not be ideal tracers for the dynamics of the galaxy as a ...the dynamical mass ...galaxy evolution until dense clumps collapse, at which point star ... See full document

... from young stars is absorbed by dust within galaxies and is thermally re-radiated in the far-infrared (FIR; Desert, Boulanger & Puget ...cosmic star-formation history can also be explored through ... See full document

... the star formation in the disc followed by passive evolution as the galaxy fades to an ...the star formation quenched by starvation (Larson, Tinsley & Caldwell 1980; Bekki, Shioya ... See full document

... 2005). Star clusters form within giant molecular clouds and remain em- bedded in their natal clouds for ∼2–5 Myr before the combined effect of massive stellar winds and supernovae drive out the gas not used ... See full document

... passive evolution for z ...galaxy formation history with a single formation time-scale, but rather there is a scatter in the inferred ages ...2009). Clusters at z > 1 were much more active ... See full document