Modeling Dense Star Clusters in the Milky Way and Beyond with the CMC Cluster Catalog

  title={Modeling Dense Star Clusters in the Milky Way and Beyond with the CMC Cluster Catalog},
  author={Kyle Kremer and Claire S. Ye and N Z Rui and Newlin C. Weatherford and Sourav Chatterjee and Giacomo Fragione and Carl L. Rodriguez and Mario Spera and Frederic A. Rasio},
  journal={The Astrophysical Journal Supplement Series},
We present a set of 148 independent N-body simulations of globular clusters (GCs) computed using the code CMC (Cluster Monte Carlo). At an age of ∼10–13 Gyr, the resulting models cover nearly the full range of cluster properties exhibited by the Milky Way GCs, including total mass, core and half-light radii, metallicity, and galactocentric distance. We use our models to investigate the role that stellar-mass black holes play in the process of core collapse. Furthermore, we study how dynamical… 

Formation of Low-mass Black Holes and Single Millisecond Pulsars in Globular Clusters

Close encounters between neutron stars and main-sequence stars occur in globular clusters and may lead to various outcomes. Here we study encounters resulting in the tidal disruption of the star.

Implications of Eccentric Observations on Binary Black Hole Formation Channels

Orbital eccentricity is one of the most robust discriminators for distinguishing between dynamical and isolated formation scenarios of binary black hole mergers using gravitational-wave observatories

Demographics of Triple Systems in Dense Star Clusters

Depending on the stellar type, more than 15% of stars in the field have at least two stellar companions. Hierarchical triple systems can be assembled dynamically in dense star clusters, as a result

Neutron Star–Black Hole Mergers from Gravitational-wave Captures

LIGO’s third observing run (O3) has reported several neutron star–black hole (NSBH) merger candidates. From a theoretical point of view, NSBH mergers have received less attention in the community

Populating the Upper Black Hole Mass Gap through Stellar Collisions in Young Star Clusters

Theoretical modeling of massive stars predicts a gap in the black hole (BH) mass function above ∼40–50 M ⊙ for BHs formed through single star evolution, arising from (pulsational) pair-instability

Stellar-mass black holes in young massive and open stellar clusters – V. comparisons with LIGO-Virgo merger rate densities

I study the contribution of young massive star clusters (YMCs) and open star clusters (OCs) to the present-day intrinsic merger rate density of dynamically-assembled binary black holes (BBHs). The

Gravitational Microlensing Rates in Milky Way Globular Clusters

Many recent observational and theoretical studies suggest that globular clusters (GCs) host compact object populations large enough to play dominant roles in their overall dynamical evolution. Yet

Compact Object Modeling in the Globular Cluster 47 Tucanae

The globular cluster 47 Tucanae (47 Tuc) is one of the most massive star clusters in the Milky Way and is exceptionally rich in exotic stellar populations. For several decades it has been a favorite

Matching Globular Cluster Models to Observations

As ancient, gravitationally bound stellar populations, globular clusters represent abundant, vibrant laboratories, characterized by high frequencies of dynamical interactions, coupled to complex

Fast Optical Transients from Stellar-mass Black Hole Tidal Disruption Events in Young Star Clusters

Observational evidence suggests that the majority of stars may have been born in stellar clusters or associations. Within these dense environments, dynamical interactions lead to high rates of close



2018a, arXiv e-prints

  • 2018

Redshift Evolution of the Black Hole Merger Rate from Globular Clusters

As the sensitivity of current and future gravitational-wave detectors improves, it will become possible to measure the evolution of the binary black hole merger rate with redshift. Here, we combine

Binary Black Hole Mergers from Globular Clusters: Implications for Advanced LIGO.

This Letter studies the formation of black hole binaries in an extensive collection of realistic globular cluster models and finds that the mergers of dynamically formed binaries could be detected at a rate of ∼100 per year, potentially dominating the binary black hole merger rate.

Dynamical evolution of globular clusters

One of the world's most distinguished astrophysicists presents a comprehensive theoretical treatment of the dynamical evolution of globular clusters. Lyman Spitzer's research in this field

X-ray binaries in globular clusters

It appears to be very unlikely that primordial binaries in globular clusters have evolved to produce high-luminosity X-ray sources like the four variable sources detected in observations by the Uhuru

The effect of pair-instability mass loss on black-hole mergers

Context. Mergers of two stellar-origin black holes are a prime source of gravitational waves and are under intensive investigation. One crucial ingredient in their modeling has been neglected:

The first gravitational-wave source from the isolated evolution of two stars in the 40–100 solar mass range

High-precision numerical simulations of the formation of binary black holes via the evolution of isolated binary stars are reported, providing a framework within which to interpret the first gravitational-wave source, GW150914, and to predict the properties of subsequent binary-black-hole gravitational- wave events.

Comprehensive analytic formulae for stellar evolution as a function of mass and metallicity

We present analytic formulae that approximate the evolution of stars for a wide range of mass M and metallicity Z. Stellar luminosity, radius and core mass are given as a function of age, M and Z,

Dynamical Evolution of Dense Stellar Systems