SNII enrichment and the star cluster mass function

Abstract

Changing the form of the star cluster mass function (CMF) can effectively change the upper end of the stellar initial mass function. The yields of from supernovae are very sensitive to the mass of the progenitor star. We show that by changing the parameters of the CMF, it is possible to change the yields of oxygen and magnesium by a factor of $\sim 1.5$ and of metals in general by a factor of $\sim 1.8$.

4 pages, 2 figures, submitted to MNRAS

References in corpus (6)

• Embedded Clusters in Molecular Clouds
• Galactic-Field IMFs of Massive Stars
• Evidence for a fundamental stellar upper mass limit from clustered star formation
• The Luminosity Function of Star Clusters in Spiral Galaxies
• Implications for the formation of star clusters from extra-galactic star-formation rates
• Can a "standard" Initial Mass Function explain the metal enrichment in clusters of galaxies?

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• On the Similarity between Cluster and Galactic Stellar Initial Mass Functions
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• Chemical consequences of low star formation rates: stochastically sampling the IMF
• Extremely alpha-Enriched Globular Clusters in Early-Type Galaxies: A Step towards the Dawn of Stellar Populations?
• Variations in Integrated Galactic Initial Mass Functions due to Sampling Method and Cluster Mass Function
• Chemical and Photometric Evolution of the Local Group Galaxy NGC 6822 in a Cosmological Context
• Chemical Abundances of Globular Clusters in NGC 5128 (Centaurus A)
• Galactic consequences of clustered star formation