scholarly journals Modeling of the Effects of Stellar Feedback during Star Cluster Formation Using a Hybrid Gas and N-Body Method

2020 ◽  
Vol 904 (2) ◽  
pp. 192 ◽  
Author(s):  
Joshua E. Wall ◽  
Mordecai-Mark Mac Low ◽  
Stephen L. W. McMillan ◽  
Ralf S. Klessen ◽  
Simon Portegies Zwart ◽  
...  
Keyword(s):  
Cluster Formation ◽  
Star Cluster ◽  
Stellar Feedback ◽  
Body Method

scholarly journals Implementing Primordial Binaries in Simulations of Star Cluster Formation with a Hybrid MHD and Direct N-Body Method

2020 ◽  
Author(s):  
Claude Cournoyer-Cloutier ◽  
Aaron Tran ◽  
Sean Lewis ◽  
Joshua E Wall ◽  
William E Harris ◽  
...  
Keyword(s):  
Binary Systems ◽  
Binary Star ◽  
Cluster Formation ◽  
Dynamical Evolution ◽  
Star Cluster ◽  
Initial Population ◽  
Mass Ratios ◽  
Low Mass ◽  
Initial Distributions ◽  
Body Method

Abstract The fraction of stars in binary systems within star clusters is important for their evolution, but what proportion of binaries form by dynamical processes after initial stellar accretion remains unknown. In previous work, we showed that dynamical interactions alone produced too few low-mass binaries compared to observations. We therefore implement an initial population of binaries in the coupled MHD and direct N-body star cluster formation code Torch. We compare simulations with, and without, initial binary populations and follow the dynamical evolution of the binary population in both sets of simulations, finding that both dynamical formation and destruction of binaries take place. Even in the first few million years of star formation, we find that an initial population of binaries is needed at all masses to reproduce observed binary fractions for binaries with mass ratios above the q ≥ 0.1 detection limit. Our simulations also indicate that dynamical interactions in the presence of gas during cluster formation modify the initial distributions towards binaries with smaller primary masses, larger mass ratios, smaller semi-major axes and larger eccentricities. Systems formed dynamically do not have the same properties as the initial systems, and systems formed dynamically in the presence of an initial population of binaries differ from those formed in simulations with single stars only. Dynamical interactions during the earliest stages of star cluster formation are important for determining the properties of binary star systems.

scholarly journals STAR CLUSTER FORMATION WITH STELLAR FEEDBACK AND LARGE-SCALE INFLOW

2015 ◽  
Vol 815 (1) ◽  
pp. 68 ◽  
Author(s):  
Christopher D. Matzner ◽  
Peter H. Jumper
Keyword(s):  
Large Scale ◽  
Cluster Formation ◽  
Star Cluster ◽  
Stellar Feedback

scholarly journals Effects of initial density profiles on massive star cluster formation in giant molecular clouds

2021 ◽  
Author(s):  
Yingtian Chen ◽  
Hui Li ◽  
Mark Vogelsberger
Keyword(s):  
Angular Momentum ◽  
Star Formation ◽  
Molecular Clouds ◽  
Globular Clusters ◽  
Cluster Formation ◽  
Initial Density ◽  
Giant Molecular Clouds ◽  
Density Profiles ◽  
Stellar Feedback ◽  
Gas Accretion

Abstract We perform a suite of hydrodynamic simulations to investigate how initial density profiles of giant molecular clouds (GMCs) affect their subsequent evolution. We find that the star formation duration and integrated star formation efficiency of the whole clouds are not sensitive to the choice of different profiles but are mainly controlled by the interplay between gravitational collapse and stellar feedback. Despite this similarity, GMCs with different profiles show dramatically different modes of star formation. For shallower profiles, GMCs first fragment into many self-gravitation cores and form sub-clusters that distributed throughout the entire clouds. These sub-clusters are later assembled ‘hierarchically’ to central clusters. In contrast, for steeper profiles, a massive cluster is quickly formed at the center of the cloud and then gradually grows its mass via gas accretion. Consequently, central clusters that emerged from clouds with shallower profiles are less massive and show less rotation than those with the steeper profiles. This is because 1) a significant fraction of mass and angular momentum in shallower profiles is stored in the orbital motion of the sub-clusters that are not able to merge into the central clusters 2) frequent hierarchical mergers in the shallower profiles lead to further losses of mass and angular momentum via violent relaxation and tidal disruption. Encouragingly, the degree of cluster rotations in steeper profiles is consistent with recent observations of young and intermediate-age clusters. We speculate that rotating globular clusters are likely formed via an ‘accretion’ mode from centrally-concentrated clouds in the early Universe.

scholarly journals Physics and modes of star cluster formation

2009 ◽  
Vol 5 (S266) ◽  
pp. 29-34
Author(s):  
Matthew R. Bate
Keyword(s):  
Radiative Transfer ◽  
Magnetic Fields ◽  
Cluster Formation ◽  
Star Cluster ◽  
Hydrodynamical Simulations ◽  
Made In

AbstractI review the progress made in understanding the physics and modes of star cluster formation through the use of direct self-gravitating hydrodynamical simulations, including those that have recently been performed incorporating radiative transfer and magnetic fields.

scholarly journals Clues to Nuclear Star Cluster Formation from Edge?on Spirals

2006 ◽  
Vol 132 (6) ◽  
pp. 2539-2555 ◽  
Author(s):  
Anil C. Seth ◽  
Julianne J. Dalcanton ◽  
Paul W. Hodge ◽  
Victor P. Debattista
Keyword(s):  
Cluster Formation ◽  
Star Cluster

scholarly journals Shock-induced star cluster formation in colliding galaxies

2010 ◽  
Vol 6 (S270) ◽  
pp. 483-486 ◽  
Author(s):  
Takayuki R. Saitoh ◽  
Hiroshi Daisaka ◽  
Eiichiro Kokubo ◽  
Junichiro Makino ◽  
Takashi Okamoto ◽  
...  
Keyword(s):  
High Resolution ◽  
Shock Compression ◽  
Smoothed Particle Hydrodynamics ◽  
Formation Process ◽  
Cluster Formation ◽  
Star Clusters ◽  
Star Cluster ◽  
Particle Hydrodynamics ◽  
Smoothed Particle ◽  
Number Of Particles

AbstractWe studied the formation process of star clusters using high-resolutionN-body/smoothed particle hydrodynamics simulations of colliding galaxies. The total number of particles is 1.2×108for our high resolution run. The gravitational softening is 5 pc and we allow gas to cool down to ~10 K. During the first encounter of the collision, a giant filament consists of cold and dense gas found between the progenitors by shock compression. A vigorous starburst took place in the filament, resulting in the formation of star clusters. The mass of these star clusters ranges from 105−8M⊙. These star clusters formed hierarchically: at first small star clusters formed, and then they merged via gravity, resulting in larger star clusters.

scholarly journals Massive Star Cluster Formation and Destruction in Luminous Infrared Galaxies in GOALS. II. An ACS/WFC3 Survey of Nearby LIRGs

2021 ◽  
Vol 923 (2) ◽  
pp. 278
Author(s):  
S. T. Linden ◽  
A. S. Evans ◽  
K. Larson ◽  
G. C. Privon ◽  
L. Armus ◽  
...  
Keyword(s):  
Hubble Space Telescope ◽  
Early Stage ◽  
Cluster Formation ◽  
Age Distribution ◽  
Star Clusters ◽  
Star Cluster ◽  
Wide Field ◽  
Infrared Galaxies ◽  
Luminous Infrared Galaxies ◽  
Cluster Age

Abstract We present the results of a Hubble Space Telescope WFC3 near-UV and Advanced Camera for Surveys Wide Field Channel optical study into the star cluster populations of a sample of 10 luminous infrared galaxies (LIRGs) in the Great Observatories All-Sky LIRG Survey. Through integrated broadband photometry we have derived ages, masses, and extinctions for a total of 1027 star clusters in galaxies with d L < 110 Mpc in order to avoid issues related to cluster bending. The measured cluster age distribution slope of dN / d τ ∝ τ − 0.5 + / − 0.12 is steeper than what has been observed in lower-luminosity star-forming galaxies. Further, differences in the slope of the observed cluster age distribution between inner- ( dN / d τ ∝ τ − 1.07 + / − 0.12 ) and outer-disk ( dN / d τ ∝ τ − 0.37 + / − 0.09 ) star clusters provide evidence of mass-dependent cluster destruction in the central regions of LIRGs driven primarily by the combined effect of strong tidal shocks and encounters with massive giant molecular clouds. Excluding the nuclear ring surrounding the Seyfert 1 nucleus in NGC 7469, the derived cluster mass function (CMF; dN / dM ∝ M α ) offers marginal evidence for a truncation in the power law at M t ∼ 2×106 M ⊙ for our three most cluster-rich sources, which are all classified as early stage mergers. Finally, we find evidence of a flattening of the CMF slope of dN / dM ∝ M − 1.42 ± 0.1 for clusters in late-stage mergers relative to early stage (α = −1.65 ± 0.02), which we attribute to an increase in the formation of massive clusters over the course of the interaction.

scholarly journals Star cluster formation in Orion A

2020 ◽  
Author(s):  
Wanggi Lim ◽  
Fumitaka Nakamura ◽  
Benjamin Wu ◽  
Thomas G Bisbas ◽  
Jonathan C Tan ◽  
...  
Keyword(s):  
Cluster Formation ◽  
Star Cluster ◽  
The Other ◽  
Young Stellar Objects ◽  
Molecular Gas ◽  
Archival Data ◽  
Formation Processes ◽  
Collision Process ◽  
Stellar Objects ◽  
Collision Model

Abstract We introduce new analysis methods for studying the star cluster formation processes in Orion A, especially examining the scenario of a cloud–cloud collision. We utilize the CARMA–NRO Orion survey 13CO (1–0) data to compare molecular gas to the properties of young stellar objects from the SDSS III IN-SYNC survey. We show that the increase of $v_{\rm {}^{13}CO} - v_{\rm YSO}$ and Σ scatter of older YSOs can be signals of cloud–cloud collision. SOFIA-upGREAT 158 μm [C ii] archival data toward the northern part of Orion A are also compared to the 13CO data to test whether the position and velocity offsets between the emission from these two transitions resemble those predicted by a cloud–cloud collision model. We find that the northern part of Orion A, including regions ONC-OMC-1, OMC-2, OMC-3, and OMC-4, shows qualitative agreements with the cloud–cloud collision scenario, while in one of the southern regions, NGC 1999, there is no indication of such a process in causing the birth of new stars. On the other hand, another southern cluster, L 1641 N, shows slight tendencies of cloud–cloud collision. Overall, our results support the cloud–cloud collision process as being an important mechanism for star cluster formation in Orion A.

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