The effect of stellar winds on the formation of a protocluster

@article{Dale2008TheEO,
  title={The effect of stellar winds on the formation of a protocluster},
  author={James E. Dale and Ian A. Bonnell},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2008},
  volume={391},
  pages={2-13}
}
  • J. Dale, I. Bonnell
  • Published 11 August 2008
  • Physics
  • Monthly Notices of the Royal Astronomical Society
We present smoothed particle hydrodynamics simulations of protoclusters including the effects of the stellar winds from massive stars. Using a particle-injection method, we investigate the effect of structure in close proximity to the wind sources and the short-time-scale influence of winds on protoclusters. We find that the structures such as discs and gaseous filaments have a strong collimating effect on winds. By a different technique of injecting momentum from point sources into our… Expand
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References

SHOWING 1-10 OF 17 REFERENCES
The onset of collapse in turbulently supported molecular clouds
We examine the formation of bound coherent clumps within the environment of turbulent molecular clouds, with emphasis on determining the role that turbulent motions play in the star formationExpand
Relative Effects of Ionizing Radiation and Winds from O-Type Stars on the Structure and Dynamics of H ii Regions
The structure and dynamics of H ii regions (and some planetary nebulae) are affected not only by radiative heating via photoionization but also by winds from the embedded O-type stars. When a fastExpand
Star formation in transient molecular clouds
We present the results of a numerical simulation in which star formation proceeds from an initially unbound molecular cloud core. The turbulent motions, which dominate the dynamics, dissipate inExpand
Photoionizing feedback in star cluster formation
We present the first ever hydrodynamic calculations of star cluster formation that incorporate the effect of feedback from ionizing radiation. In our simulations, the ionizing source forms in theExpand
The hierarchical formation of a stellar cluster
Recent surveys of star-forming regions have shown that most stars, and probably all massive stars, are born in dense stellar clusters. The mechanism by which a molecular cloud fragments to formExpand
Interstellar bubbles. II - Structure and evolution
The detailed structure of the interaction of a strong stellar wind with the interstellar medium is presented. First, an adiabatic similarity solution is given which is applicable at early times.Expand
Accretion in stellar clusters and the collisional formation of massive stars
We present results from a numerical simulation of gas accretion in a cluster containing 1000 stars. The accretion forces the cluster to contract, leading to the development of a high-density coreExpand
Modelling accretion in protobinary systems
A method for following fragmentation simulations further in time using smoothed particle hydrodynamics (SPH) is presented. In a normal SPH simulation of the collapse and fragmentation of a molecularExpand
Rapid Formation of Molecular Clouds and Stars in the Solar Neighborhood
We show how molecular clouds in the solar neighborhood might be formed and produce stars rapidly enough to explain stellar population ages, building on results from numerical simulations of theExpand
Slow Star Formation in Dense Gas: Evidence and Implications
It has been known for more than 30 years that star formation in giant molecular clouds (GMCs) is slow, in the sense that only ~1% of the gas forms stars every free-fall time. This result is entirelyExpand
...
1
2
...