Journal Article

PUBDB-2022-06649

http://join2-wiki.gsi.de/foswiki/pub/Main/Artwork/join2_logo100x88.png Modeling Dense Star Clusters in the Milky Way and beyond with the Cluster Monte Carlo Code

Rodriguez, C. L. (Corresponding author) ; Weatherford, N. C. ; Coughlin, S. C. ; Amaro-Seoane, P.DESY* ; Breivik, K. ; Chatterjee, S. ; Fragione, G. ; Kıroğlu, F. ; Kremer, K. ; Rui, N. Z. ; Ye, C. S. ; Zevin, M. ; Rasio, F. A.

2022
Univ. of Chicago Press Chicago, Ill. [u.a.]

This record in other databases:        

Please use a persistent id in citations: doi:10.3847/1538-4365/ac2edf  doi:10.3204/PUBDB-2022-06649

Report No.: arXiv:2106.02643

Abstract: We describe the public release of the Cluster Monte Carlo (CMC) code, a parallel, star-by-star N-body code for modeling dense star clusters. CMC treats collisional stellar dynamics using Hénon’s method, where the cumulative effect of many two-body encounters is statistically reproduced as a single effective encounter between nearest-neighbor particles on a relaxation timescale. The star-by-star approach allows for the inclusion of additional physics, including strong gravitational three- and four-body encounters, two-body tidal and gravitational-wave captures, mass loss in arbitrary galactic tidal fields, and stellar evolution for both single and binary stars. The public release of CMC is pinned directly to the COSMIC population synthesis code, allowing dynamical star cluster simulations and population synthesis studies to be performed using identical assumptions about the stellar physics and initial conditions. As a demonstration, we present two examples of star cluster modeling: first, we perform the largest (N = 10$^{8}$) star-by-star N-body simulation of a Plummer sphere evolving to core collapse, reproducing the expected self-similar density profile over more than 15 orders of magnitude; second, we generate realistic models for typical globular clusters, and we show that their dynamical evolution can produce significant numbers of black hole mergers with masses greater than those produced from isolated binary evolution (such as GW190521, a recently reported merger with component masses in the pulsational pair-instability mass gap).

Note: ISSN 1538-4365 not unique: **2 hits**.Code is available at https://clustermontecarlo.github.io/ 25 pages, 8 Figures, Matches version accepted by ApJS

---

Contributing Institute(s):

1. Theoretische Astroteilchenphysik (Z_THAT)

Research Program(s):

1. 611 - Fundamental Particles and Forces (POF4-611) (POF4-611)

Experiment(s):

1. No specific instrument

Appears in the scientific report 2022

---

Database coverage:
; ; Clarivate Analytics Master Journal List ; Current Contents - Physical, Chemical and Earth Sciences ; Essential Science Indicators ; IF >= 5 ; JCR ; SCOPUS ; Science Citation Index Expanded ; Web of Science Core Collection

---

---

Linked articles:

http://join2-wiki.gsi.de/foswiki/pub/Main/Artwork/join2_logo100x88.png Preprint Rodriguez, C. L. (Corresponding author) ; Weatherford, N. C. ; Coughlin, S. C. ; Amaro-Seoane, P. ; Breivik, K. ; Chatterjee, S. ; Fragione, G. ; Kıroğlu, F. ; Kremer, K. ; Rui, N. Z. ; Ye, C. S. ; Zevin, M. ; Rasio, F. A.
Modeling Dense Star Clusters in the Milky Way and beyond with the Cluster Monte Carlo Code
[10.3204/PUBDB-2022-06889]     Files  Fulltext by arXiv.org BibTeX | EndNote: XML, Text | RIS

---