Hierarchical formation of Westerlund 1: a collapsing cluster with no primordial mass segregation?

Gennaro, Mario; Goodwin, S. P.; Parker, R. J.; Allison, Richard J.; Brandner, W.

doi:10.1093/mnras/stx2098

Cited by 17 publications

(15 citation statements)

References 66 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The first few to 10s of Myrs of cluster evolution likely feature various complex processes such as hierarchical mergers and residual gas expulsion. Indeed, such processes are hinted at from observations of several young massive clusters (e.g., Kuhn et al 2014;Gennaro et al 2017). In particular, residual gas expulsion could lead to significant cluster expansion at early times, attenuating the long-term dynamical processing of BHs and thus altering the structural features of the clusters at late times.…”

Section: Discussionmentioning

confidence: 99%

The Role of “black hole burning” in the evolution of dense star clusters

Kremer

Chatterjee

et al. 2019

Proc. IAU

View full text Add to dashboard Cite

As self-gravitating systems, dense star clusters exhibit a natural diffusion of energy from their innermost to outermost regions, leading to a slow and steady contraction of the core until it ultimately collapses under gravity. However, in spite of the natural tendency toward “core collapse,” the globular clusters (GCs) in the Milky Way exhibit a well-observed bimodal distribution in core radii separating the core-collapsed and non-core-collapsed clusters. This suggests an internal energy source is at work, delaying the onset of core collapse in many clusters. Over the past decade, a large amount of work has suggested that stellar black holes (BHs) play a dynamically-significant role in clusters throughout their entire lifetimes. Here we review our latest understanding of BH populations in GCs and demonstrate that, through their dynamical interaction with their host cluster, BHs can naturally explain the distinction between core-collapsed and non-core-collapsed clusters through a process we call “black hole burning.”

show abstract

Section: Discussionmentioning

confidence: 99%

The Role of “black hole burning” in the evolution of dense star clusters

Kremer

Chatterjee

et al. 2019

Proc. IAU

View full text Add to dashboard Cite

show abstract

“…Young star clusters show signs of mass segregation (Hillenbrand & Hartmann, 1998;de Grijs et al, 2002;Littlefair et al, 2003;Stolte et al, 2005Stolte et al, , 2006Kim et al, 2006;Harayama et al, 2008;Espinoza et al, 2009;Bontemps et al, 2010;Gennaro et al, 2011). However, observations of pre-main sequence stars in star-forming regions do not indicate mass segregation (Parker et al, 2011(Parker et al, , 2012Gennaro et al, 2017;Parker & Alves de Oliveira, 2017;Dib et al, 2018). Plunkett et al (2018) find the prestellar cores in Serpens South to be mass-segregated, whereas the pre-main sequence stars are not.…”

Section: Mass Segregation In Young Clustersmentioning

confidence: 96%

The Physics of Star Cluster Formation and Evolution

Krause¹,

Offner²,

Charbonnel³

et al. 2020

Space Sci Rev

107

View full text Add to dashboard Cite

Star clusters form in dense, hierarchically collapsing gas clouds. Bulk kinetic energy is transformed to turbulence with stars forming from cores fed by filaments. In the most compact regions, stellar feedback is least effective in removing the gas and stars may form very efficiently. These are also the regions where, in high-mass clusters, ejecta from some kind of high-mass stars are effectively captured during the formation phase of some of the low mass stars and effectively channeled into the latter to form multiple populations. Star formation epochs in star clusters are generally set by gas flows that determine the abundance of gas in the cluster. We argue that there is likely only one star formation epoch after which clusters remain essentially clear of gas by cluster winds. Collisional dynamics is important in this phase leading to core collapse, expansion and eventual dispersion of every cluster. We review recent developments in the field with a focus on theoretical work.

show abstract

“…With ∼ 5 × 10 4 M (Gennaro et al 2017, and references therein), Westerlund 1 (Wd1) is the most massive YSC in the Milky Way. With an age of ∼ 5 Myr it has already undergone several supernova explosions and is dynamically more evolved than other, younger massive Milky Way star clusters (m > 10 4 M ), such as Westerlund 2 (Wd2, Westerlund 1961) or NGC 3603.…”

Section: Young Massive Star Clusters In the Milky Way And Magellanic Cloudsmentioning

confidence: 99%

Star Clusters Near and Far

et al. 2020

View full text Add to dashboard Cite

Star clusters are fundamental units of stellar feedback and unique tracers of their host galactic properties. In this review, we will first focus on their constituents, i.e. detailed insight into their stellar populations and their surrounding ionised, warm, neutral, and molecular gas. We, then, move beyond the Local Group to review star cluster populations at various evolutionary stages, and in diverse galactic environmental conditions accessible in the local Universe. At high redshift, where conditions for cluster formation and evolution are more extreme, we are only able to observe the integrated light of a handful of objects that we believe will become globular clusters. We therefore discuss how numerical and analytical methods, informed by the observed properties of cluster populations in the local Universe, are used to develop sophisticated simulations potentially capable of disentangling the genetic map of galaxy formation and assembly that is carried by globular cluster populations.

show abstract

Hierarchical formation of Westerlund 1: a collapsing cluster with no primordial mass segregation?

Cited by 17 publications

References 66 publications

The Role of “black hole burning” in the evolution of dense star clusters

The Role of “black hole burning” in the evolution of dense star clusters

The Physics of Star Cluster Formation and Evolution

Star Clusters Near and Far

Contact Info

Product

Resources

About