The Chemical Evolution of Globular Clusters I. Reactive Elements and Non-Metals - Astrophysics > Astrophysics of GalaxiesReportar como inadecuado




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Abstract: We propose a new chemical evolution model aimed at explaining the chemicalproperties of globular clusters GC stars. Our model depends upon theexistence of i a peculiar pre-enrichment phase in the GC-s parent galaxyassociated with very low-metallicity Type II supernovae SNeII, and iilocalized inhomogeneous enrichment from a single Type Ia supernova SNeIa andintermediate-mass 4 7Msun asymptotic giant branch AGB field stars. GCformation is then assumed to take place within this chemically-peculiar region.Thus, in our model the first low-mass GC stars to form are those with peculiarabundances i.e., O-depleted and Na-enhanced while ``normal- stars i.e.,O-rich and Na depleted are formed in a second stage when self-pollution fromSNeII occurs and the peculiar pollution from the previous phase is dispersed.In this study, we focus on three different GCs: NGC6752, NGC6205 M13 andNGC2808. We demonstrate that, within this framework, a model can be constructedwhich is consistent with i the elemental abundance anti-correlations, iiisotopic abundance patterns, and iii the extreme O-Fe values observed inNGC2808 and M13, without violating the global constraints of approximatelyunimodal Fe-H and C+N+O.



Autor: Andrea Marcolini UCLan, Brad K. Gibson UCLan, Amanda I. Karakas Mt Stromlo, Patricia Sanchez-Blazquez UCLan, IAC

Fuente: https://arxiv.org/



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