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Chemical abundance ...
Chemical abundance analysis of the extremely metal-poor star HE 1300+0157
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Frebel, Anna (författare)
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Norris, John E. (författare)
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Aoki, Wako (författare)
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visa fler...
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Honda, Satoshi (författare)
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Bessell, Michael S. (författare)
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Takada-Hidai, Masahide (författare)
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Beers, Timothy C. (författare)
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- Christlieb, Norbert (författare)
- Uppsala universitet,Institutionen för astronomi och rymdfysik
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visa färre...
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(creator_code:org_t)
- 2007
- 2007
- Engelska.
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Ingår i: Astrophysical Journal. - 0004-637X .- 1538-4357. ; 658:1, s. 534-552
- Relaterad länk:
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https://urn.kb.se/re...
Abstract
Ämnesord
Stäng
- We present a detailed chemical abundance analysis of HE 1300+0157, a subgiant with Fe/H = -3.9. Froma high-resolution, high-S/N Subaru HDS spectrum we find the star to be enriched in C ([C/Fe](1D) similar to +1.4) and O ([O/Fe](1D) similar to +1.8). With the exception of these species, HE 1300+0157 exhibits an elemental abundance pattern similar to that found in many other very and extremely metal-poor stars. The Li abundance is lower than the Spite plateau value, in agreement with expectation for its evolutionary status. Of particular interest, no neutron-capture elements are detected in HE 1300+0157. This type of abundance pattern has been found by recent studies in several other metal-poor giants. We suggest that HE 1300+0157 is an unevolved example of this group of stars, which exhibit high C abundances together with low (or absent) abundances of neutron-capture elements (CEMP-no). Several potential enrichment scenarios are presented. The nondetection of neutron-capture elements including Sr, Ba, and Pb suggests that the carbon excess observed in HE 1300+0157 is not due to mass transfer across a binary system. Such a scenario is applied to carbon-rich objects with excesses of s-process elements. The normal observed Li abundance supports this interpretation. Most likely, the high levels of C and O were produced prior to the birth of this star. It remains unclear whether a single faint SN is responsible for its overall chemical pattern, or whether one requires a superposition of yields from a massive Population III object and a hypernova. These scenarios provide important information on the C production in the early universe and on the formation of C-rich stars in the early Galaxy.
Ämnesord
- NATURVETENSKAP -- Fysik (hsv//swe)
- NATURAL SCIENCES -- Physical Sciences (hsv//eng)
Nyckelord
- Galaxy : abundances
- Galaxy : halo
- stars : abundances
- stars : individual (HE 1300+0157)
- stars : Population II
- Physics
- Fysik
Publikations- och innehållstyp
- ref (ämneskategori)
- art (ämneskategori)
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