Numerical Simulations of Globular Cluster Formation

Abstract

We examine various physical processes associated with the formation of globular clusters by using the three-dimensional Smoothed Particle Hydrodynamics (SPH) code. Our code includes radiative cooling of gases, star formation, energy feedback from stars including stellar winds and supernovae, and chemical enrichment by stars. We assume that, in the collapsing galaxy, isothermal cold clouds form through thermal condensations and become proto-globular clouds. We calculate the size of proto-globular clouds by solving the linearized equations for perturbation. We compute the evolution of the inner region of the proto-cloud with our SPH code for various initial radius and initial composition of gases. When the initial gases contain no heavy elements, the evolution of proto-clouds sensitively depends on the initial radius. For a smaller initial radius, the initial star burst is so intense that the subsequent star formation occurs in the central regions to form a dense star cluster as massive as the globular cluster. When the initial gases contain some heavy elements, the metallicity of gases affects the evolution and the final stellar mass. If the initial radius of the proto-globular clouds was relatively large, the formation of a star cluster as massive as the globular clusters requires the initial metallicity as high as [Fe/H] $\ge -2$. The self-enrichment of heavy elements in the star cluster does not occur in all cases.

Accpeted for publication in the ApJ. Correctiong errors in Table 1

References in corpus (4)

• Nucleosynthesis in Type II Supernovae
• The Evolution of Dwarf Galaxies with Star Formation in Outward Propagating Super Shell
• Dissipative Process as a Mechanism of Differentiating Internal Structures between Dwarf and Normal Elliptical Galaxies in a CDM Universe
• Smoothed Particle Hydrodynamics with GRAPE and Parallel Virtual Machine

Cited by in corpus (22)

• Formation of globular clusters in hierarchical cosmology
• Paving the way for the JWST: witnessing globular cluster formation at z>3
• Mg isotopic ratios in giant stars of the globular cluster NGC 6752
• The Formation of the First Globular Clusters in Dwarf Galaxies Before the Epoch of Reionization
• Formation of Multiple Populations in Globular Clusters: Another Possible Scenario
• Formation of Second Generation Stars in Globular Clusters
• 3-D Simulations of the Chemical and Dynamical Evolution of the Galactic Bulge
• Globular cluster systems II: On the formation of old globular clusters and their sites of formation
• Insights into Pre-Enrichment of Star Clusters and Self-Enrichment of Dwarf Galaxies from their Intrinsic Metallicity Dispersions
• Globular cluster formation with multiple stellar populations: self-enrichment in fractal massive molecular clouds
• Massive stars and globular cluster formation
• Formation of Compact Stellar Clusters by High-Redshift Galaxy Outflows I: Nonequillibrium Coolant Formation
• Self-consistent simulations of star cluster formation from gas clouds under the influence of galaxy-scale tidal fields
• The First Billion Years Project: Finding Infant Globular Clusters at z=6
• Triggering the Formation of Halo Globular Clusters with Galaxy Outflows
• Stellar cluster formation in a Milky Way-sized galaxy at z>4 -- I. The proto-globular cluster population and the imposter amongst us
• Formation of Compact Stellar Clusters by High-Redshift Galaxy Outflows II: Effect of Turbulence and Metal-Line Cooling
• Metal Enrichment of The Primordial Interstellar Medium through 3-D Hydrodynamical Evolution of The First Supernova Remnant
• Formation of Globular Clusters in Turbulent Molecular Clouds
• Extragalactic Star Clusters: Speculations on the Future
• Linking the Internal Properties of Infant Globular Clusters to their Formation Environments
• An efficient method for calculation of cooling in Lagrange computational gas dynamics