Superbubble dynamics in globular cluster infancy - II. Consequences for secondary star formation in the context of self-enrichment via fast-rotating massive stars
Martin Krause,Corinne Charbonnel,Corinne Charbonnel,Thibaut Decressin,Georges Meynet,Nikos Prantzos +5 more
TLDR
In this paper, the authors studied the interaction of fast-rotating massive stars (FRMS) with the intra-cluster medium (ICM) and developed a timeline of the first ≈40 Myr of GC evolution.Abstract:
Context. The self-enrichment scenario for globular clusters (GC) requires large amounts of residual gas after the initial formation of the first stellar generation. Recently, we found that supernovae may not be able to expel that gas, as required to explain their presentday gas-free state, and suggested that a sudden accretion onto the dark remnants at a stage when type II supernovae have ceased may plausibly lead to fast gas expulsion. Aims. Here, we explore the consequences of these results for the self-enrichment scenario via fast-rotating massive stars (FRMS). Methods. We analysed the interaction of FRMS with the intra-cluster medium (ICM), in particular where, when, and how the second generation of stars may form. From the results, we developed a timeline of the first ≈40 Myr of GC evolution. Results. Our previous results imply three phases during which the ICM is in a fundamentally different state, namely the wind bubble phase (lasting 3. 5t o 8.8 Myr), the supernova phase (lasting 26. 2t o 31.5 Myr), and the dark remnant accretion phase (lasting 0. 1t o 4 Myr): (i) Quickly after the first-generation massive stars have formed, stellar wind bubbles compress the ICM into thin filaments. No stars may form in the normal way during this phase because of the high Lyman-Werner flux density. If the first-generation massive stars have equatorial ejections however, as we proposed in the FRMS scenario, accretion may resume in the shadow of the equatorial ejecta. The second-generation stars may then form due to gravitational instability in these disc, which are fed by both the FRMS ejecta and pristine gas. (ii) In the supernova phase the ICM develops strong turbulence, with characteristic velocities below the escape velocity. The gas does not accrete either onto the stars or onto the dark remnants in this phase because of the high gas velocities. The strong mass loss associated with the transformation of the FRMS into dark remnants then leads to the removal of the secondgeneration stars from the immediate vicinity of the dark remnants. (iii) When the supernovae have ceased, turbulence quickly decays, and the gas can once more accrete, now onto the dark remnants. As discussed previously, this may release sufficient energy to unbind the gas, and may happen fast enough so that a large fraction of less tightly bound first-generation stars are lost. Conclusions. Studying the FRMS scenario for the self-enrichment of GCs in detail reveals the important role of the physics of the ICM for our understanding of the formation and early evolution of GCs. Depending on the level of mass segregation, this sets constraints on the orbital properties of the stars, in particular high orbital eccentricities, which likely has implications on the GC formation scenario.read more
Citations
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Journal ArticleDOI
The Hubble Space TelescopeUV Legacy Survey of Galactic Globular Clusters – V. Constraints on formation scenarios
Alvio Renzini,Francesca D'Antona,Santi Cassisi,I. R. King,Antonino Milone,Paolo Ventura,Jonathan Anderson,Luigi R. Bedin,Andrea Bellini,Thomas M. Brown,Giampaolo Piotto,R. P. van der Marel,Beatriz Barbuy,Emanuele Dalessandro,Sebastian L. Hidalgo,Sebastian L. Hidalgo,Anna F. Marino,Sergio Ortolani,Maurizio Salaris,Ata Sarajedini +19 more
TL;DR: In this paper, the authors build on the evidence provided by their Legacy Survey of Galactic globular clusters (GC) to submit to a crucial test four scenarios currently entertained for the formation of multiple stellar generations in GCs.
Journal ArticleDOI
Globular clusters as the relics of regular star formation in ‘normal’ high-redshift galaxies
TL;DR: In this paper, an end-to-end, two-phase model for the origin of globular clusters (GCs) is presented, where populations of stellar clusters form in the high-pressure discs of high-redshift ($z>2$) galaxies (a rapid-disruption phase due to tidal perturbations from the dense interstellar medium), after which the galaxy mergers associated with hierarchical galaxy formation redistribute the surviving, massive clusters into the galaxy haloes, where they remain until the present day.
Journal ArticleDOI
Globular cluster formation in the context of galaxy formation and evolution
TL;DR: In this article, the formation of massive, GC progenitor clusters is restricted to high-pressure environments similar to those observed at high redshift and at the sites of YMC formation in the local Universe.
Journal ArticleDOI
A general abundance problem for all self-enrichment scenarios for the origin of multiple populations in globular clusters
TL;DR: In this article, a consistency check between the results of fitting extreme cases with the requirements of more typical clusters has been done, focusing mainly on Na, O and He, and it was shown that any enrichment source that can fit clusters like NGC 2808, will necessarily fail (by construction) to fit more typical cluster like 47 Tuc or NGC 288.
Journal ArticleDOI
Concurrent formation of supermassive stars and globular clusters: implications for early self-enrichment
Mark Gieles,Corinne Charbonnel,Corinne Charbonnel,Martin Krause,Vincent Hénault-Brunet,Vincent Hénault-Brunet,Oscar Agertz,Henny J. G. L. M. Lamers,Nate Bastian,Alessia Gualandris,Alice Zocchi,J. A. Petts +11 more
TL;DR: In this paper, a model for the concurrent formation of globular clusters (GCs) and supermassive stars (SMSs, ≳103 M⊙) is presented to address the origin of the HeCNONaMgAl abundance anomalies in GCs.
References
More filters
Journal ArticleDOI
Energy input from quasars regulates the growth and activity of black holes and their host galaxies
TL;DR: Simulations that simultaneously follow star formation and the growth of black holes during galaxy–galaxy collisions find that, in addition to generating a burst of star formation, a merger leads to strong inflows that feed gas to the supermassive black hole and thereby power the quasar.
Journal ArticleDOI
Disk Frequencies and Lifetimes in Young Clusters
TL;DR: In this paper, the authors report the results of the first sensitive L-band survey of the intermediate-age (2.5-30 Myr) clusters NGC 2264, NGC 2362, and NGC 1960.
Journal ArticleDOI
Interstellar bubbles. II - Structure and evolution
TL;DR: In this article, the detailed structure of the interaction of a strong stellar wind with the interstellar medium is presented, including the effects of thermal conduction between the hot interior and the cold shell of swept-up interstellar matter.