Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005omeg.conf..466o&link_type=abstract
ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2003. Held 17-19 November 2003 in RIKEN, Wako, Saitama, Japan. Edited by M Terasawa,
Astronomy and Astrophysics
Astronomy
Scientific paper
We studied Mg isotope ratios in globular-cluster stars using a simple supernova-induced self-enrichment model. Our basic idea is to explain the observed Mg isotope ratios by the contribution from an early generation of intermediate-mass stars. Although our model produces some Mg isotopic abundance variation, not enough heavier Mg isotopes (25Mg and 26Mg) were formed unless star formation occurs in low density regions behind the super shell. In our model, the 1st generation of AGB stars could not affect heavier Mg isotopes if we assume contamination occurs in the super shell. We also discuss neutron-capture elements in M15 using the same model. It appears difficult to explain current observational results by cloud-collision models. If we assume the r-process occurs in low-mass supernovae, (e.g., ONeMg supernovae), our self-enrichment model can reproduce the observed [Ba/Fe] scatter.
Ashenfelter Timothy
Mathews Grant J.
Otsuki Kaori
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