Can star cluster environment affect dust input from massive AGB stars?

Abstract

We examine the fraction of massive asymptotic giant branch (AGB) stars remaining bound in their parent star clusters and the effect of irradiation of these stars by intracluster ultraviolet (UV) field. We employ a set of N-body models of dynamical evolution of star clusters rotating in a galactic potential at the solar galactocentric radius. The cluster models are combined with stellar evolution formulae, a library of stellar spectra, and simple models for SiO photodissociation in circumstellar environment (CSE). The initial stellar masses of clusters are varied from $50{\mathrm{M}}_{\odot }$ to $10^5{\mathrm{M}}_{\odot }$. Results derived for individual clusters are combined using a mass distribution function for young star clusters. We find that about 30% of massive AGB stars initially born in clusters become members of the field population, while the rest evolves in star clusters. They are irradiated by strong intracluster UV radiation resulting in the decrease of the photodissociation radius of SiO molecules, in many stars down to the dust formation zone. In absence of dust shielding, the UV photons penetrate in the CSE deeper than $10R_{\ast }$ in 64% and deeper than $2R_{\ast }$ in 42% of all massive AGB stars. If this suppresses following dust formation, the current injection rate of silicate dust from AGB stars in the local Galaxy decreases from $2.2\times 10^{-4}{\mathrm{M}}_{\odot }\mathrm{kp}{\mathrm{c}}^{-2}\mathrm{Gy}{\mathrm{r}}^{-1}$ to $1.8\times 10^{-4}{\mathrm{M}}_{\odot }\mathrm{kp}{\mathrm{c}}^{-2}\mathrm{Gy}{\mathrm{r}}^{-1}$ at most. A lower revised value of 40% for the expected fraction of presolar silicate grains from massive AGB stars is still high to explain the non-detection of these grains in meteorites.

accepted to ApJ, 14 pages, 9 figures, 5 tables

References in corpus (25)

• A comprehensive set of simulations studying the influence of gas expulsion on star cluster evolution
• Evolution of interstellar dust and stardust in the solar neighbourhood
• Photoprocesses in protoplanetary disks
• Super and Massive AGB Stars: II - Nucleosynthesis and Yields - Z=0.02, 0.008 and 0.004
• Aluminum-, Calcium- And Titanium-Rich Oxide Stardust In Ordinary Chondrite Meteorites
• Probing the role of the galactic environment in the formation of stellar clusters; using M83 as a test bench
• Performance Analysis of Direct N-Body Algorithms on Special-Purpose Supercomputers
• Evolution of Thermally Pulsing Asymptotic Giant Branch Stars II. Dust production at varying metallicity
• Destruction of Interstellar Dust in Evolving Supernova Remnant Shock Waves
• The mmax-Mecl relation, the IMF and IGIMF: probabilistically sampled functions?
• Evidence for primordial mass segregation in globular clusters
• UV Radiation Fields Produced by Young Embedded Star Clusters
• Dust origin in late-type dwarf galaxies: ISM growth vs. type II supernovae
• Dense Stellar Populations: Initial Conditions
• ACS imaging of star clusters in M51. I. Identification and radius distribution
• Hot bottom burning and s-process nucleosynthesis in massive AGB stars at the beginning of the thermally-pulsing phase
• No evidence for mass segregation in massive young clusters
• Constraining globular cluster formation through studies of young massive clusters - III. A lack of gas and dust in massive stellar clusters in the LMC and SMC
• New reaction rate for 16O(p,gamma)17F and its influence on the oxygen isotopic ratios in massive AGB stars
• Shape parameters of Galactic open clusters
• Ejection of globular cluster interstellar media through ionization by white dwarfs
• The evolution of the global stellar mass function of star clusters: an analytic description
• The wind of W Hya as seen by Herschel. II. The molecular envelope of W Hya
• Can the third dredge-up extinguish hot-bottom burning in massive AGB stars?
• The spatial distribution of substellar objects in IC348 and the Orion Trapezium Cluster

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• Iron and silicate dust growth in the Galactic interstellar medium: clues from element depletions
• The ALMA detection of CO rotational line emission in AGB stars in the Large Magellanic Cloud
• The photodissociation of CO in circumstellar envelopes
• The rotational disruption of porous dust aggregates from ab-initio kinematic calculations