English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

(abridged) We consider the effect of stellar remnants on the interstellarmedium of a massive star cluster following the initial burst of star formation.We argue that accretion onto stellar-mass black holes (BHs) is an effectivemechanism for rapid gas depletion in clusters of all masses, as long as theycontain progenitor stars more massive than \gtrsim 50\msun. This scenario isattractive for the progenitor systems of present-day massive globular clusters(GCs) which likely had masses M \gtrsim 10^7\msun. In such clusters, supernovaeand stellar winds cannot provide a plausible explanation for the sudden removalof the primordial gas reservoir that is required to explain their complexchemical enrichment history.  In order to consider different regimes in the gas accretion rate ontostellar-mass BHs, we consider both the Bondi-Hoyle and Eddingtonapproximations. For either model, our results show that the gas can besignificantly depleted within only a few tens of Myrs. This process will affectthe distribution of BH masses, and may accelerate the dynamical decoupling ofthe BH population and, ultimately, their dynamical ejection. Moreover, thetimescales for gas depletion are sufficiently short that the accreting BHscould significantly affect the chemistry of subsequent star formation episodes.  The gas depletion times and final mass in BHs are sensitive to the assumedmodel for the accretion rate, and to the initial mass of the most massive BHwhich, in turn, is determined by the upper mass cut-off of the stellar IMF. Ourresults imply that the remnant accretion history can have an important bearingon the observed present-day cluster mass-to-light ratio. In particular, we showthat an increase of the upper mass cut-off with decreasing metallicity couldcontribute to the observed anti-correlation between the mass-to-light ratio andthe metallicity of GCs.

Gas depletion in primordial globular clusters due to accretion onto stellar-mass black holes