Formation of stellar clusters
arXiv:1709.08948 · doi:10.1093/mnras/stx2396
Abstract
We investigate the triggering of star formation and the formation of stellar clusters in molecular clouds that form as the ISM passes through spiral shocks. The spiral shock compresses gas into 100 pc long main star formation ridge, where clusters forming every 5-10 pc along the merger ridge. We use a gravitational potential based cluster finding algorithm, which extracts individual clusters, calculates their physical properties and traces cluster evolution over multiple time steps. Final cluster masses at the end of simulation range between 1000 and 30000 M with their characteristic half-mass radii between 0.1 pc and 2 pc. These clusters form by gathering material from 10-20 pc size scales. Clusters also show a mass - specific angular momentum relation, where more massive clusters have larger specific angular momentum due to the larger size scales, and hence angular momentum from which they gather their mass. The evolution shows that more massive clusters experiences hierarchical merging process, which increases stellar age spreads up to 2-3 Myr. Less massive clusters appear to grow by gathering nearby recently formed sinks, while more massive clusters with their large global gravitational potentials are increasing their mass growth from gas accretion.
10 pages; 13 figures
References in corpus (23)
- A Spitzer Survey of Young Stellar Clusters within One Kiloparsec of the Sun: Cluster Core Extraction and Basic Structural Analysis
- On the onset of galactic winds in quiescent star forming galaxies
- Before the first supernova: combined effects of HII regions and winds on molecular clouds
- ATLASGAL --- towards a complete sample of massive star forming clumps
- On the Rapid Collapse and Evolution of Molecular Clouds
- The Spatial Structure of Young Stellar Clusters. I. Subclusters
- Kinematic Structure of the Orion Nebula Cluster and its Surroundings
- The formation of molecular clouds in spiral galaxies
- A cluster in the making: ALMA reveals the initial conditions for high-mass cluster formation
- Driven and Decaying Turbulence Simulations of Low-Mass Star Formation: From Clumps to Cores to Protostars
- Dependency of dynamical ejections of O stars on the masses of very young star clusters
- Spatial Distributions of Young Stars
- The formation of NGC 3603 young starburst cluster: "prompt" hierarchical assembly or monolithic starburst?
- The bound fraction of young star clusters
- The W43-MM1 mini-starburst ridge, a test for star formation efficiency models
- Core-Halo Age Gradients and Star Formation in the Orion Nebula and NGC~2024 Young Stellar Clusters
- Tracing the Conversion of Gas into Stars in Young Massive Cluster Progenitors
- The Spatial Structure of Young Stellar Clusters. II. Total Young Stellar Populations
- Stellar clusterings around "Isolated" Massive YSOs in the LMC
- Captured older stars as the reason for apparently prolonged star formation in young star clusters
- The IMF as a function of supersonic turbulence
- Photoionising feedback and the star formation rates in galaxies
- Models for the Formation of Massive Stars