Complete ejection of OB stars from very young star clusters and the formation of multiple populations

@article{Wang2018CompleteEO,
  title={Complete ejection of OB stars from very young star clusters and the formation of multiple populations},
  author={Long Wang and Pavel Kroupa and Tereza Jeř{\'a}bkov{\'a}},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2018}
}
Recently, three stellar sequences separated in age by about 1 Myr were discovered in the Orion Nebula Cluster (ONC; Beccari et al. 2017). Kroupa et al. (2018) suggest that such small dense subpopulations eject all their OB stars via the decay of unstable few-body systems such that the gas can recombine and form new stars. This explains the multisequence phenomenon without introducing an extra mechanism into star formation theory. In this work, we apply the recently updated primordial binary… 

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References

SHOWING 1-10 OF 59 REFERENCES

Evidence for feedback and stellar-dynamically regulated bursty star cluster formation: the case of the Orion Nebula Cluster

(abridged) A scenario for the formation of multiple co-eval populations separated in age by about 1 Myr in very young clusters (VYCs, ages less than 10 Myr) and with masses in the range 600-20000

A highly abnormal massive star mass function in the Orion Nebula cluster and the dynamical decay of trapezium systems

The Orion Nebula cluster (ONC) appears to be unusual on two grounds: the observed constellation of the OB stars of the entire ONC and its Trapezium at its centre implies a time-scale problem given

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

STELLAR CLUSTERINGS AROUND “ISOLATED” MASSIVE YSOs IN THE LMC

Observations suggest that there is a significant fraction of O stars in the field of the Milky Way that appear to have formed in isolation or in low-mass clusters (<100 ). The existence of these

Inverse dynamical population synthesis: Constraining the initial conditions of young stellar clusters by studying their binary populations

Binary populations in young star clusters show multiplicit y fractions both lower and up to twice as high as those observed in the Galactic field. We follow the evolution of a population of bin ary

Is stellar multiplicity universal? Tight stellar binaries in the Orion nebula Cluster

We present a survey for the tightest visual binaries among 0.3–2 M⊙ members of the Orion nebula Cluster (ONC). Among 42 targets, we discovered 13 new 0.025–0.15 arcsec companions. Accounting for the

DEPENDENCY OF DYNAMICAL EJECTIONS OF O STARS ON THE MASSES OF VERY YOUNG STAR CLUSTERS

Massive stars can be efficiently ejected from their birth star clusters through encounters with other massive stars. We study how the dynamical ejection fraction of O star systems varies with the

CATCH ME IF YOU CAN: IS THERE A “RUNAWAY-MASS” BLACK HOLE IN THE ORION NEBULA CLUSTER?

We investigate the dynamical evolution of the Orion Nebula Cluster (ONC) by means of direct N-body integrations. A large fraction of residual gas was probably expelled when the ONC formed, so we

N‐body simulations of stars escaping from the Orion nebula

We study the dynamical interaction in which the two single runaway stars, AE Aurigae and mu Columbae, and the binary iota Orionis acquired their unusually high space velocity. The two single runaways

The stellar and sub-stellar IMF of simple and composite populations

The current knowledge on the stellar IMF is documented. It appears to become top-heavy when the star-formation rate density surpasses about 0.1Msun/(yr pc^3) on a pc scale and it may become
...