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Computation of Atmospheric Concentrations of Molecular Clusters from ab initio Thermochemistry

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Published on: April 8, 2020

Young and intermediate-age massive star clusters.

Søren S Larsen¹

¹Astronomical Institute, University of Utrecht, Princetonplein 5, 3584 CC Utrecht, The Netherlands. s.s.laren@uu.nl

Philosophical Transactions. Series A, Mathematical, Physical, and Engineering Sciences

|January 20, 2010

Summary

This summary is machine-generated.

Star clusters form in dense gas clouds, dispersing quickly or remaining bound. Massive clusters survive for cosmic timescales, while low-mass clusters are common but less durable.

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Area of Science:

Astronomy
Astrophysics
Cosmic Evolution

Background:

Star clusters form within dense molecular gas clouds.
Cluster evolution depends on star formation efficiency and gas clearing.
Dissolution occurs through internal relaxation and external shocks.

Purpose of the Study:

To provide an overview of star cluster formation and evolution.
To emphasize the characteristics of high-mass star clusters.
To discuss the factors influencing cluster lifetimes and mass distributions.

Main Methods:

Review of current observational and theoretical understanding.
Analysis of cluster mass functions and survival timescales.
Comparison of cluster formation in different galactic environments.

Main Results:

Low-mass clusters follow a power-law mass distribution.
Massive clusters (>10^5 M☉) can survive for cosmological timescales.
Starburst galaxies and globular cluster systems form more massive clusters than quiescent spiral discs.

Conclusions:

Cluster dispersal is influenced by initial conditions and environmental factors.
Massive cluster formation is linked to high gas densities and pressures, characteristic of violent star formation.
Low-mass clusters may indicate universal star formation, while massive clusters highlight specific energetic events.