Modeling Dense Star Clusters in the Milky Way and Beyond with the $texttt{CMC}$ Cluster Catalog. (arXiv:1911.00018v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kremer_K/0/1/0/all/0/1">Kyle Kremer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ye_C/0/1/0/all/0/1">Claire S. Ye</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rui_N/0/1/0/all/0/1">Nicholas Z. Rui</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weatherford_N/0/1/0/all/0/1">Newlin C. Weatherford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chatterjee_S/0/1/0/all/0/1">Sourav Chatterjee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fragione_G/0/1/0/all/0/1">Giacomo Fragione</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_C/0/1/0/all/0/1">Carl L. Rodriguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Spera_M/0/1/0/all/0/1">Mario Spera</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rasio_F/0/1/0/all/0/1">Frederic A. Rasio</a>
We present a set of 148 independent $N$-body simulations of globular clusters
(GCs) computed using the code $texttt{CMC}$ ($texttt{Cluster Monte Carlo}$).
At an age of $sim10-13,$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 interactions
affect the formation and evolution of several important types of sources in
GCs, including low-mass X-ray binaries, millisecond pulsars, blue stragglers,
cataclysmic variables, Type Ia supernovae, calcium-rich transients, and merging
compact binaries. While our focus here is on old, low-metallicity GCs, our
$texttt{CMC}$ simulations follow the evolution of clusters over a Hubble time,
and they include a wide range of metallicities (up to solar), so that our
results can also be used to study younger and higher-metallicity star clusters.
We present a set of 148 independent $N$-body simulations of globular clusters
(GCs) computed using the code $texttt{CMC}$ ($texttt{Cluster Monte Carlo}$).
At an age of $sim10-13,$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 interactions
affect the formation and evolution of several important types of sources in
GCs, including low-mass X-ray binaries, millisecond pulsars, blue stragglers,
cataclysmic variables, Type Ia supernovae, calcium-rich transients, and merging
compact binaries. While our focus here is on old, low-metallicity GCs, our
$texttt{CMC}$ simulations follow the evolution of clusters over a Hubble time,
and they include a wide range of metallicities (up to solar), so that our
results can also be used to study younger and higher-metallicity star clusters.
http://arxiv.org/icons/sfx.gif
