Stellar-mass Black Holes in Globular Clusters: Dynamical consequences and observational signatures

Abbas Askar, Mirek Giersz, Manuel Arca Sedda, Ammar Askar, Mario Pasquato, Agostino Leveque

    Research output: Contribution to journalArticlepeer-review


    Sizeable number of stellar-mass black holes (BHs) in globular clusters (GCs) can strongly influence the dynamical evolution and observational properties of their host cluster. Using results from a large set of numerical simulations, we identify the key ingredients needed to sustain a sizeable population of BHs in GCs up to a Hubble time. We find that while BH natal kick prescriptions are essential in determining the initial retention fraction of BHs in GCs, the long-Term survival of BHs is determined by the size, initial central density and half-mass relaxation time of the GC. Simulated GC models that contain many BHs are characterized by relatively low central surface brightness, large half-light and core radii values. We also discuss novel ways to compare simulated results with available observational data to identify GCs that are most likely to contain many BHs.

    Original languageEnglish (US)
    Pages (from-to)395-399
    Number of pages5
    JournalProceedings of the International Astronomical Union
    Issue number351
    StatePublished - 2019


    • globular clusters: general
    • stars: black holes
    • stellar dynamics

    ASJC Scopus subject areas

    • Astronomy and Astrophysics
    • Space and Planetary Science


    Dive into the research topics of 'Stellar-mass Black Holes in Globular Clusters: Dynamical consequences and observational signatures'. Together they form a unique fingerprint.

    Cite this