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dc.contributor.authorHerwig, Falk
dc.contributor.authorVandenBerg, Don A.
dc.contributor.authorNavarro, Julio F.
dc.contributor.authorFerguson, Jason W.
dc.contributor.authorPaxton, Bill
dc.date.accessioned2012-11-01T21:06:27Z
dc.date.available2012-11-01T21:06:27Z
dc.date.issued2012-10-01
dc.identifier.citationHerwig, Falk; VandenBerg, Don A.; Navarro, Julio F.; Ferguson, Jason; Paxton, Bill. 2012. From the color-magnitude diagram of omega centauri and (super-) asymptotic giant branch stellar models to a galactic plane passage gas purging chemical evolution scenario. Astrophysical Journal, v.757 no.2 art.132en_US
dc.identifier.issn0004-637X
dc.identifier.otherWOS:000309108500025
dc.identifier.urihttp://dx.doi.org/10.1088/0004-637X/757/2/132
dc.identifier.urihttp://hdl.handle.net/10057/5343
dc.descriptionClick on the DOI link to access the article (may not be free).en_US
dc.description.abstractWe have investigated the color-magnitude diagram of omega Centauri and find that the blue main sequence (bMS) can be reproduced only by models that have a helium abundance in the range Y = 0.35-0.40. To explain the faint subgiant branch of the reddest stars ("MS-a/RG-a" sequence), isochrones for the observed metallicity ([Fe/H] approximate to -0.7) appear to require both a high age (similar to 13 Gyr) and enhanced CNO abundances ([CNO/Fe] approximate to 0.9). Y approximate to 0.35 must also be assumed in order to counteract the effects of high CNO on turnoff colors and thereby to obtain a good fit to the relatively blue turnoff of this stellar population. This suggests a short chemical evolution period of time (<1 Gyr) for omega Cen. Our intermediate-mass (super-) asymptotic giant branch (AGB) models are able to reproduce the high helium abundances, along with [N/Fe] similar to 2 and substantial O depletions if uncertainties in the treatment of convection are fully taken into account. These abundance features distinguish the bMS stars from the dominant [Fe/H] approximate to -1.7 population. The most massive super-AGB stellar models (M-ZAMS >= 6.8M(circle dot), M-He,M-core >= 1.245M(circle dot)) predict too large N enhancements, which limit their role in contributing to the extreme populations. In order to address the observed central concentration of stars with He-rich abundance, we show here quantitatively that highly He- and N-enriched AGB ejecta have particularly efficient cooling properties. Based on these results and on the reconstruction of the orbit of omega Cen with respect to the Milky Way, we propose the Galactic plane passage gas purging scenario for the chemical evolution of this cluster. The bMS population formed shortly after the purging of most of the cluster gas as a result of the passage of omega Cen through the Galactic disk (which occurs today every similar to 40 Myr for omega Cen) when the initial mass function of the dominant population had "burned" through most of the Type II supernova mass range. AGB stars would eject most of their masses into the gas-depleted cluster through low-velocity winds that sink to the cluster core due to their favorable cooling properties and form the bMS population. In our discussion we follow our model through four passage events, which could explain some key properties not only of the bMS but also of the MS-a/RGB-a and the s-enriched stars.en_US
dc.language.isoen_USen_US
dc.publisherIOP Publishingen_US
dc.relation.ispartofseriesAstrophysical Journal;v.757 no.2
dc.subjectGlobular clusters: individual (omega Cen)en_US
dc.subjectHertzsprung-Russell and C-M diagramsen_US
dc.subjectStarsen_US
dc.subjectAbundancesen_US
dc.subjectEvolutionen_US
dc.titleFrom the color-magnitude diagram of omega centauri and (super-) asymptotic giant branch stellar models to a galactic plane passage gas purging chemical evolution scenarioen_US
dc.typeArticleen_US
dc.description.versionPeer reviewed
dc.rights.holderCopyright American Astronomical Society (AAS), 2012


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