Matches in SemOpenAlex for { <https://semopenalex.org/work/W2103367868> ?p ?o ?g. }
- W2103367868 endingPage "340" @default.
- W2103367868 startingPage "304" @default.
- W2103367868 abstract "Photospheric abundances are presented for 27 elements from carbon to europium in 181 F and G dwarfs from a differential local thermodynamic equilibrium (LTE) analysis of high-resolution and high signal-to-noise ratio spectra. Stellar effective temperatures (Teff) were adopted from an infrared flux method calibration of Strömgren photometry. Stellar surface gravities (g) were calculated from Hipparcos parallaxes and stellar evolutionary tracks. Adopted Teff and g values are in good agreement with spectroscopic estimates. Stellar ages were determined from evolutionary tracks. Stellar space motions (U, V, W) and a Galactic potential were used to estimate Galactic orbital parameters. These show that the vast majority of the stars belong to the Galactic thin disc. Relative abundances expressed as [X/Fe] generally confirm previously published results. We give results for C, N, O, Na, Mg, Al, Si, S, K, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Cu, Zn, Sr, Y, Zr, Ba, Ce, Nd and Eu. The α elements — O, Mg, Si, Ca and Ti — show [α/Fe] to increase slightly with decreasing [Fe/H]. Heavy elements with dominant contributions at solar metallicity from the s-process show [s/Fe] to decrease slightly with decreasing [Fe/H]. Scatter in [X/Fe] at a fixed [Fe/H] is entirely attributable to the small measurement errors, after excluding the few thick disc stars and the s-process-enriched CH subgiants. Tight limits are set on ‘cosmic’ scatter. If a weak trend with [Fe/H] is taken into account, the composition of a thin disc star expressed as [X/Fe] is independent of the star's age and birthplace for elements contributed in different proportions by massive stars (Type II supernovae), exploding white dwarfs (Type Ia supernovae) and asymptotic red giant branch stars. By combining our sample with various published studies, comparisons between thin and thick disc stars are made. In this composite sample, thick disc stars are primarily identified by their VLSR in the range −40 to −100 km s−1. These are very old stars with origins in the inner Galaxy and metallicities [Fe/H]≤−0.4. At the same [Fe/H], the sampled thin disc stars have VLSR∼ 0 km s−1, and are generally younger with a birthplace at about the Sun's Galactocentric distance. In the range −0.35 ≥[Fe/H]≥−0.70, well represented by present thin and thick disc samples, [X/Fe] of the thick disc stars is greater than that of thin disc stars for Mg, Al, Si, Ca, Ti and Eu. [X/Fe] is very similar for the thin and thick disc for — notably — Na and iron-group elements. Barium ([Ba/Fe]) may be underabundant in thick relative to thin disc stars. These results extend previous ideas about composition differences between the thin and thick disc." @default.
- W2103367868 created "2016-06-24" @default.
- W2103367868 creator A5020600710 @default.
- W2103367868 creator A5027387088 @default.
- W2103367868 creator A5029732789 @default.
- W2103367868 creator A5090865138 @default.
- W2103367868 date "2003-03-21" @default.
- W2103367868 modified "2023-10-16" @default.
- W2103367868 title "The chemical compositions of Galactic disc F and G dwarfs" @default.
- W2103367868 cites W1659875532 @default.
- W2103367868 cites W1965561594 @default.
- W2103367868 cites W1966653725 @default.
- W2103367868 cites W1967911932 @default.
- W2103367868 cites W1970936861 @default.
- W2103367868 cites W1972078212 @default.
- W2103367868 cites W1975818093 @default.
- W2103367868 cites W1982159507 @default.
- W2103367868 cites W1983395404 @default.
- W2103367868 cites W1995204717 @default.
- W2103367868 cites W1996589776 @default.
- W2103367868 cites W2012595831 @default.
- W2103367868 cites W2016268550 @default.
- W2103367868 cites W2020138278 @default.
- W2103367868 cites W2026278684 @default.
- W2103367868 cites W2026673826 @default.
- W2103367868 cites W2029263067 @default.
- W2103367868 cites W2043258333 @default.
- W2103367868 cites W2045268462 @default.
- W2103367868 cites W2047228913 @default.
- W2103367868 cites W2050114676 @default.
- W2103367868 cites W2062281103 @default.
- W2103367868 cites W2069801284 @default.
- W2103367868 cites W2083189282 @default.
- W2103367868 cites W2083724380 @default.
- W2103367868 cites W2092680751 @default.
- W2103367868 cites W2094928710 @default.
- W2103367868 cites W2101798377 @default.
- W2103367868 cites W2106648118 @default.
- W2103367868 cites W2107002261 @default.
- W2103367868 cites W2109138120 @default.
- W2103367868 cites W2143307438 @default.
- W2103367868 cites W2146066087 @default.
- W2103367868 cites W2157402710 @default.
- W2103367868 cites W2157594202 @default.
- W2103367868 cites W2160299852 @default.
- W2103367868 cites W2165031544 @default.
- W2103367868 cites W3098498583 @default.
- W2103367868 cites W3102923143 @default.
- W2103367868 cites W3105270778 @default.
- W2103367868 cites W3121389110 @default.
- W2103367868 cites W3124101725 @default.
- W2103367868 cites W3124275756 @default.
- W2103367868 cites W4231599316 @default.
- W2103367868 cites W4292406868 @default.
- W2103367868 doi "https://doi.org/10.1046/j.1365-8711.2003.06305.x" @default.
- W2103367868 hasPublicationYear "2003" @default.
- W2103367868 type Work @default.
- W2103367868 sameAs 2103367868 @default.
- W2103367868 citedByCount "672" @default.
- W2103367868 countsByYear W21033678682012 @default.
- W2103367868 countsByYear W21033678682013 @default.
- W2103367868 countsByYear W21033678682014 @default.
- W2103367868 countsByYear W21033678682015 @default.
- W2103367868 countsByYear W21033678682016 @default.
- W2103367868 countsByYear W21033678682017 @default.
- W2103367868 countsByYear W21033678682018 @default.
- W2103367868 countsByYear W21033678682019 @default.
- W2103367868 countsByYear W21033678682020 @default.
- W2103367868 countsByYear W21033678682021 @default.
- W2103367868 countsByYear W21033678682022 @default.
- W2103367868 countsByYear W21033678682023 @default.
- W2103367868 crossrefType "journal-article" @default.
- W2103367868 hasAuthorship W2103367868A5020600710 @default.
- W2103367868 hasAuthorship W2103367868A5027387088 @default.
- W2103367868 hasAuthorship W2103367868A5029732789 @default.
- W2103367868 hasAuthorship W2103367868A5090865138 @default.
- W2103367868 hasBestOaLocation W21033678681 @default.
- W2103367868 hasConcept C121332964 @default.
- W2103367868 hasConcept C1276947 @default.
- W2103367868 hasConcept C150846664 @default.
- W2103367868 hasConcept C172119930 @default.
- W2103367868 hasConcept C174802034 @default.
- W2103367868 hasConcept C44870925 @default.
- W2103367868 hasConcept C4839761 @default.
- W2103367868 hasConcept C68271606 @default.
- W2103367868 hasConcept C85837739 @default.
- W2103367868 hasConcept C98444146 @default.
- W2103367868 hasConcept C99465377 @default.
- W2103367868 hasConceptScore W2103367868C121332964 @default.
- W2103367868 hasConceptScore W2103367868C1276947 @default.
- W2103367868 hasConceptScore W2103367868C150846664 @default.
- W2103367868 hasConceptScore W2103367868C172119930 @default.
- W2103367868 hasConceptScore W2103367868C174802034 @default.
- W2103367868 hasConceptScore W2103367868C44870925 @default.
- W2103367868 hasConceptScore W2103367868C4839761 @default.
- W2103367868 hasConceptScore W2103367868C68271606 @default.
- W2103367868 hasConceptScore W2103367868C85837739 @default.
- W2103367868 hasConceptScore W2103367868C98444146 @default.