Volume 597, January 2017
|Number of page(s)||15|
|Section||Galactic structure, stellar clusters and populations|
|Published online||19 December 2016|
How can young massive clusters reach their present-day sizes?
1 Argelander-Institut für Astronomie (AIfA), Auf dem Hügel 71, 53121 Bonn, Germany
2 Helmholtz-Instituts für Strahlen- und Kernphysik (HISKP), Nussallee 14-16, 53115 Bonn, Germany
Received: 9 July 2015
Accepted: 13 October 2015
Context. The classic question of how young massive star clusters attain the shapes and sizes, as we find them today, is still a difficult one. Both observational and computational studies of star-forming massive molecular gas clouds suggest that massive cluster formation is primarily triggered along the small-scale (≲0.3 pc) filamentary substructures within the clouds.
Aims. The present study investigates the possible ways in which a filament-like, compact, massive star cluster (effective radius 0.1−0.3 pc) can expand more than 10 times, still remaining massive enough (≳ 104M⊙) to become the young massive star cluster that we observe today.
Methods. To this end, model massive clusters (initially 104−105M⊙) are evolved using Sverre Aarseth’s state-of-the-art N-body code NBODY7. Apart from the accurate calculation of two-body relaxation of the constituent stars, these evolutionary models take into account stellar-evolutionary mass loss and dynamical energy injection due to massive, tight primordial binaries and stellar-remnant black holes and neutron stars. These calculations also include a solar-neighbourhood-like external tidal field. All the computed clusters expand with time, and their sizes (effective radii) are compared with those observed for young massive clusters (≲ 100 Myr) in the Milky Way and other nearby galaxies.
Results. In this study, it is found that beginning from the above compact sizes, a star cluster cannot expand on its own, i.e., due to two-body relaxation, stellar mass loss, and dynamical heating by primordial binaries and compact stars up to the observed sizes of young massive clusters; star clusters always remain much more compact than the observed ones.
Conclusions. This calls for additional mechanisms that boost the expansion of a massive cluster after its assembly. Using further N-body calculations, it is shown that a substantial residual gas expulsion with ≈ 30% star formation efficiency can indeed swell the newborn embedded cluster adequately. The limitations of the present calculations and their consequences are discussed.
Key words: galaxies: star clusters: general / methods: numerical / star: formation / stars: kinematics and dynamics
© ESO, 2016
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