2018/12/31 by Michiko S. Fujii, M. S. Fujii
Physics and Astronomy · #Astro and Planetary Science #Astrophysics #Astrophysics and Star Formation Studies #Cluster (spacecraft) #Galaxy #Molecular cloud #Nebula #Orion Nebula #Physics #Star (game theory) #Star cluster #Star formation #Stars #Stellar, planetary, and galactic studies #Velocity dispersion #astro-ph.GA
paper · pdf · doi:10.1093/mnras/stz1056
9 pages, 5 figures, MNRAS accepted
arxiv created 2019/04/11 · openalex publication_date 2019/04/12 · arxiv updated 2019/04/24 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Star cluster complexes such as the Carina Nebula could have formed in turbulent giant molecular clouds. We perform a series of N-body simulations starting from subclustering initial conditions based on hydrodynamic simulations of turbulent molecular clouds. These simulations finally result in the formation of star cluster complexes consisting of several subclusters (clumps). We obtain the inter-clump velocity distribution, the size of the region, and the mass of the most massive cluster in our simulated complex and compare the results with observed ones (the Carina Nebula and NGC 2264). The one-dimensional inter-clump velocity dispersion obtained from our simulations is 2.9 ± 0.3 and 1.4 ± 0.4 km s−1 for the Carina- and NGC 2264-like models, respectively, which are consistent with those obtained from Gaia Data Release 2: 2.35 and 0.99 km s−1 for the Carina Nebula and NGC 2264, respectively. We estimate that the masses of the parental molecular clouds for the Carina Nebula and the NGC 2264 are 4 × 105 and |4× 104 M\odot |, respectively.