Stellar Collisions and the Interior Structure of Blue Stragglers

@article{Lombardi2002StellarCA,
  title={Stellar Collisions and the Interior Structure of Blue Stragglers},
  author={J. Lombardi and J. S. Warren and F. Rasio and A. Sills and Aaron R. Warren},
  journal={The Astrophysical Journal},
  year={2002},
  volume={568},
  pages={939-953}
}
  • J. Lombardi, J. S. Warren, +2 authors Aaron R. Warren
  • Published 2002
  • Physics
  • The Astrophysical Journal
  • Collisions of main-sequence stars occur frequently in dense star clusters. In open and globular clusters, these collisions produce merger remnants that may be observed as blue stragglers. Detailed theoretical models of this process require lengthy hydrodynamic computations in three dimensions. However, a less computationally expensive approach, which we present here, is to approximate the merger process (including shock heating, hydrodynamic mixing, mass ejection, and angular momentum transfer… CONTINUE READING

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    References

    Publications referenced by this paper.
    SHOWING 1-10 OF 36 REFERENCES
    Smoothed particle hydrodynamics
    • 4,012
    • PDF
    Theory of rotating stars
    • 650
    • Highly Influential
    Blue Stragglers and Other Stellar Anomalies: Implications for the Dynamics of Globular Clusters
    • 181
    BINARIES IN GLOBULAR-CLUSTERS
    • 283
    • PDF
    Evolution of Stellar Collision Products in Globular Clusters - II. Off-axis Collisions.
    • 79
    • PDF
    Stellar Collisions in Globular Clusters and the Blue Straggler Problem
    • 107
    The evolution of rotating stars. I - Method and exploratory calculations for a 7-solar-mass star
    • 169
    • Highly Influential