Synthetic properties of models of globular clusters

Angeletti, L.; Dolcetta, R. Capuzzo; Giannone, P.

doi:10.1007/bf00638964

Cited by 13 publications

(7 citation statements)

References 19 publications

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“…As expected, and as already noted by e.g. Angeletti et al (1980), the contribution of the WD population to optical and NIR photometric indices is negligible, although they contribute to the total mass of the cluster significantly.…”

Section: Ingredientssupporting

confidence: 89%

Monte Carlo simulations of metal-poor star clusters

Fagiolini

Raimondo

Degl’Innocenti

2006

A&A

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Context. Metal-poor globular clusters (GCs) can provide a probe of the earliest epoch of star formation in the Universe, being the oldest observable stellar systems. In addition, young and intermediate-age low-metallicity GCs are present in external galaxies. Nevertheless, inferring their evolutionary status by using integrated properties may suffer from large intrinsic uncertainty caused by the discrete nature of stars in stellar systems, especially in the case of faint objects. Aims. In this paper, we evaluate the intrinsic uncertainty (due to statistical effects) affecting the integrated colours and mass-to-light ratios as a function of the cluster's integrated visual magnitude (M tot V ), which represents a directly measured quantity. We investigate the case of metal-poor, single-burst stellar populations with age from a few million years to a likely upper value for the Galactic globular cluster ages (∼15 Gyr). Methods. Our approach is based on Monte Carlo techniques for randomly generating stars distributed according to the cluster's mass function. Results. Integrated colours and mass-to-light ratios in different photometric bands are checked for good agreement with the observational values of low-metallicity Galactic clusters; the effect of different assumptions on the horizontal branch (HB) morphology is shown to be irrelevant, at least for the photometric bands explored here. We present integrated colours and mass-to-light ratios as a function of age for different assumptions on the cluster total V magnitude. We find that the intrinsic uncertainty cannot be neglected. In particular, in models with M tot V = −4 the broad-band colours show an intrinsic uncertainty high enough to prevent the precise age of the cluster from being evaluated. The effects of different assumptions on the initial mass function and on the minimum mass for which carbon burning is ignited for both integrated colours and mass-to-light ratios are also analysed. Finally, the present predictions are compared with recent results available in the literature, showing non-negligible differences in some cases.

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Section: Ingredientssupporting

confidence: 89%

Monte Carlo simulations of metal-poor star clusters

Fagiolini

Raimondo

Degl’Innocenti

2006

A&A

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“…It has long been debated whether mass-loss by stellar winds and/or supernovae (SNe) is efficient in affecting core collapse (e.g. Angeletti & Giannone 1977, 1980Applegate 1986;Chernoff & Shapiro 1987;Chernoff & Weinberg 1990;Hurley et al 2004;Schulman et al 2012;Downing 2012;Sippel et al 2012). In fact, stellar winds and SNe eject mass from a SC, making the central potential well shallower and quenching the onset of gravothermal instability.…”

Section: The Impact Of Three-body Encounters and Stellar Evolution On...mentioning

confidence: 99%

Impact of metallicity on the evolution of young star clusters

Mapelli

Bressan

2013

Monthly Notices of the Royal Astronomical Society

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The early evolution of a dense young star cluster (YSC) depends on the intricate connection between stellar evolution and dynamical processes. Thus, Nbody simulations of YSCs must account for both aspects. We discuss N-body simulations of YSCs with three different metallicities (Z = 0.01, 0.1 and 1 Z ⊙ ), including metallicity-dependent stellar evolution recipes and metallicity-dependent prescriptions for stellar winds and remnant formation. We show that mass-loss by stellar winds influences the reversal of core collapse. In particular, the post-collapse expansion of the core is faster in metal-rich YSCs than in metal-poor YSCs, because the former lose more mass (through stellar winds) than the latter. As a consequence, the half-mass radius expands more in metal-poor YSCs. We also discuss how these findings depend on the total mass and on the virial radius of the YSC. These results give us a clue to understand the early evolution of YSCs with different metallicity.

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“…Two recognised key parameters for estimating tGW are: (1) the initial protogalactic radius (which sets the binding energy of the system), and (2) the evolution of the thermal energy content of the SNe remnants. The former has been addressed by Angeletti & Giannone (1991) and the latter by Gibson (1994), and are not wholly relevant for the discussion which follows as we will simply adopt the formalism used by BCF94.…”

Section: Introductionmentioning

confidence: 99%

Stellar mass-loss-driven wind models of elliptical galaxies?

Gibson

1994

Monthly Notices of the Royal Astronomical Society

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Recent claims in the literature ) that the epoch describing the onset of galactic winds in spheroidal star systems has been severely overestimated in the past, due to the neglect of energy deposited in the interstellar medium from stellar winds, is evaluated in the light of a more conservative approach to modeling the input of thermal energy to the system from massive stars undergoing mass loss. Applying the most recent models of stellar kinetic energy deposition, coupled with reasonable assumptions regarding the e ciency of thermalisation, it is shown that contrary to the aforementioned study, the in uence of stellar winds in driving the galactic winds in ellipticals of M G > 10 9 M is most likely negligible.

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Synthetic properties of models of globular clusters

Cited by 13 publications

References 19 publications

Monte Carlo simulations of metal-poor star clusters

Monte Carlo simulations of metal-poor star clusters

Impact of metallicity on the evolution of young star clusters

Stellar mass-loss-driven wind models of elliptical galaxies?

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