Diluting the material forming the second generation stars in Globular Clusters: the contribution by unevolved stars

Abstract

In this short communication we consider the possibility that stars less evolved than the polluters are the source of the dilution needed to explain the observed composition of second-generation globular cluster (GC) stars and the Na-O and Mg-Al anticorrelations. If these stars can lose 0.5-1% of their mass during the relevant epochs, there is enough diluting material to produce the observed anticorrelations. In this case, the original mass of proto-GCs was several tens times higher than the current mass of GCs. While not strictly impossible, this is a stringent hypothesis that needs more support. Should this scenario be found true, then the link between the primordial (first-generation) population in GC and the field population would be very strong.

Accepted for publication on Astronomy and Astrophysics

References in corpus (9)

• Fast rotating massive stars and the origin of the abundance patterns in galactic globular clusters
• Formation and Dynamical Evolution of Multiple Stellar Generations in Globular Clusters
• Scaled solar tracks and isochrones in a large region of the Z-Y plane I. From the ZAMS to the TP-AGB end for 0.15 - 2.5 Mo stars
• On the self-enrichment scenario of galactic globular clusters: Constraints on the IMF
• The influence of residual gas expulsion on the evolution of the Galactic globular cluster system and the origin of the Population II halo
• Theoretical mass loss rates of cool main-sequence stars
• The shape of the initial cluster mass function: what it tells us about the local star formation efficiency
• Lithium abundances in red giants of M4: evidence for asymptotic giant branch star pollution in globular clusters?
• Updated Pre-Main Sequence tracks at low metallicities for 0.1< M/Mo<1.5

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• Modelling the chemical evolution of the Galaxy halo
• Models for the lithium abundances of multiple populations in globular clusters and the possible role of the Big Bang lithium
• Bayesian Analysis of Two Stellar Populations in Galactic Globular Clusters III: Analysis of 30 Clusters
• Formation of globular clusters with multiple stellar populations from massive gas clumps in high-z gas-rich dwarf galaxies
• Globular cluster formation with multiple stellar populations: A single-binary composite scenario