Pre-supernova feedback sets the star cluster mass function to a power law and reduces the cluster formation efficiency

Andersson, Eric P.; Mac Low, Mordecai-Mark; Agertz, Oscar; Renaud, Florent; Li, Hui

doi:10.1051/0004-6361/202347792

Cited by 7 publications

(1 citation statement)

References 131 publications

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“…Such a short formation time would pose a problem for the massive binaries to release their enriched material in time to be relevant. On the other hand, simulations of massive star cluster formation suggest that star formation durations up to 20 Myr (Andersson et al 2024) are possible, with many simulations suggesting that about 10 Myr is needed to assemble massive clusters (e.g., Howard et al 2018;Rizzuti et al 2023). Dating very young stars is notoriously difficult, and simulations include different prescriptions for important physical processes.…”

Section: Summary and Discussionmentioning

confidence: 99%

Massive Interacting Binaries as an Enrichment Source for Multiple Populations in Star Clusters

Nguyen,

Sills

2024

ApJ

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We present a suite of binary evolution models with massive primaries (10 ≤ M 1 ≤ 40 M ⊙) and periods and mass ratios chosen such that the systems undergo nonconservative mass transfer while the primaries have helium cores. We track the total mass and chemical composition of the ejecta from these systems. This material shows the abundance signatures of hot hydrogen burning that are needed to explain the abundance patterns seen in multiple populations in massive star clusters. We then calculate the total yield of a population of binary stars with masses, mass ratios, and periods consistent with their distribution in a field population. We show that the overall abundance of this material is enriched in helium, nitrogen, sodium, and aluminum, and depleted in carbon, oxygen, and magnesium, by amounts that are consistent with observations. We also show that such a population of binaries will return approximately 25% of its mass in this ejecta (compared to 4% if all the stars were single), over a characteristic timescale of about 12 Myr. We argue that massive binaries must be seriously considered as a contributor to the source of enriched material needed to explain the multiple populations in massive clusters, since essentially all massive stars are formed in binaries or higher-order multiples, massive binaries are primarily formed in clusters, and massive binaries naturally produce material of the right composition.

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Section: Summary and Discussionmentioning

confidence: 99%

Massive Interacting Binaries as an Enrichment Source for Multiple Populations in Star Clusters

Nguyen,

Sills

2024

ApJ

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Massive star cluster formation

Polak,

Mac Low,

Klessen

et al. 2024

A&A

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The mode of star formation that results in the formation of globular clusters and young massive clusters is difficult to constrain through observations. We present models of massive star cluster formation using the torch framework, which uses the Astrophysical MUltipurpose Software Environment (AMUSE) to couple distinct multi-physics codes that handle star formation, stellar evolution and dynamics, radiative transfer, and magnetohydrodynamics. We upgraded torch by implementing the N-body code petar thereby enabling torch to handle massive clusters forming from $10^6 M_ clouds with $ individual stars. We present results from torch simulations of star clusters forming from $10^4,\, 10^5 and\, 10^6\, M_ turbulent spherical gas clouds (named M4, M5, M6) of radius $R=11.7 pc$. We find that star formation is highly efficient and becomes more so at a higher cloud mass and surface density. For M4, M5, and M6 with initial surface densities $2.325 M_ $, after a free-fall time of $t_ ff Myr$, we find that sim 30<!PCT!>, 40<!PCT!>, and 60<!PCT!> of the cloud mass has formed into stars respectively. The end of simulation-integrated star formation efficiencies for M4, M5, and M6 are $ cloud =$36<!PCT!>, 65<!PCT!>, and 85<!PCT!>. Observations of nearby clusters similar in mass and size to M4 have instantaneous star formation efficiencies of $ inst which is slightly lower than the integrated star formation efficiency of M4. The M5 and M6 models represent a different regime of cluster formation that is more appropriate for the conditions in starburst galaxies and gas-rich galaxies at high redshift, and that leads to a significantly higher efficiency of star formation. We argue that young massive clusters build up through short efficient bursts of star formation in regions that are sufficiently dense ($ M_ $) and massive ($M_ cloud M_ In such environments stellar feedback from winds and radiation is not strong enough to counteract the gravity from gas and stars until a majority of the gas has formed into stars.

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From giant clumps to clouds

Renaud,

Agertz,

Romeo

2024

A&A

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The clumpy nature of gas-rich galaxies at cosmic noon raises the question of universality of the scaling relations and average properties of the star-forming structures. Using controlled simulations of disk galaxies and varying only the gas fraction, we show that the influence of the galactic environments (large-scale turbulence, tides, and shear) contributes, together with the different regime of instabilities, to setting a diversity of physical conditions for the formation and evolution of gas clumps from low to high gas fractions. However, the distributions of gas clumps at all gas fractions follow similar scaling relations as Larson's, suggesting the universality of median properties. Yet, we find that the scatter around these relations significantly increases with the gas fraction, allowing for the presence of massive, large, and highly turbulent clouds in gas-rich disks in addition to a more classical population of clouds. Clumps with an excess of mass for their size are slightly denser, more centrally concentrated, and host more abundant and faster star formation. We find that the star formation activity (rate, efficiency, and depletion time) correlates much more strongly with the excess of mass than with the mass itself. Our results suggest the existence of universal scaling relations for gas clumps but with redshift-dependent scatters, which calls for deeper and more complete census of the populations of star-forming clumps and young stellar clusters at cosmic noon and beyond.

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Pre-supernova feedback sets the star cluster mass function to a power law and reduces the cluster formation efficiency

Cited by 7 publications

References 131 publications

Massive Interacting Binaries as an Enrichment Source for Multiple Populations in Star Clusters

Massive Interacting Binaries as an Enrichment Source for Multiple Populations in Star Clusters

Massive star cluster formation

From giant clumps to clouds

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