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2015A&A...579A..28B - Astronomy and Astrophysics, volume 579A, 28-28 (2015/7-1)
TOPoS. II. On the bimodality of carbon abundance in CEMP stars. Implications on the early chemical evolution of galaxies.
BONIFACIO P., CAFFAU E., SPITE M., LIMONGI M., CHIEFFI A., KLESSEN R.S., FRANCOIS P., MOLARO P., LUDWIG H.-G., ZAGGIA S., SPITE F., PLEZ B., CAYREL R., CHRISTLIEB N., CLARK P.C., GLOVER S.C.O., HAMMER F., KOCH A., MONACO L., SBORDONE L. and STEFFEN M.
Abstract (from CDS):
Abstract Copyright: ∼
Journal keyword(s): that has also been enriched by a faint supernova providing carbon cloud, lighter elements. The abundance pattern of the UIP stars shows a large star-to-star scatter in the [X/Ca] ratios for all elements up to aluminium the, this scatter drops for heavier elements and is at most of the order of a factor of two. We propose that this can be explained if these stars are formed from gas that has been chemically enriched by several SNe but, produce the roughly constant [X/Ca] ratios for the heavier elements that, some cases the gas has also been polluted by the ejecta of a faint SN that contributes the lighter elements in variable amounts. The absence of lithium in four of the five known unevolved UIP stars can be explained by a dominant role of fragmentation in the formation of these stars. This would result either in a destruction of lithium in the pre-main-sequence phase, through rotational mixing or to a lack of late accretion from a reservoir of fresh gas. The phenomenon should have varying degrees of efficiency. - stars: Population II - stars: abundances - stars: Population III - Galaxy: abundances - Galaxy: formation - Galaxy: halo
VizieR on-line data: <Available at CDS (J/A+A/579/A28): stars.dat table4.dat>
CDS comments: Fig.6 HE 022-4831 is a misprint for HE 2202-4831 .
Simbad objects: 46
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