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- W2133921410 abstract "Previouscalculationsofthestatisticalequilibriumof aluminiuminthesolarphotospherehaveshownthatNLTEpop- ulations hardly affect Al line formation in the Sun; however, in metal-poor stars the influence of electron collisions is reduced, and a UV radiation eld enhanced due to smaller background line opacity results in more pronounced NLTE effects. Thus analysesbasedonNLTEpopulationsleadtosignicantlyhigher Al abundances than those calculated from LTE. For stars of in- termediate metallicity between 1:0 < (Fe/H) < 0:5 some overabundance relative to iron is found. For more metal-poor stars the overabundance disappears and approaches the solar ratio, (Al/Fe) = 0. Only a weak overabundance in the (Al/Mg) ratio is detected for stars with intermediate metallicity and a small underabundance of 0: 2t o 0 :3 dex for the metal-poor stars. From investigation of both solar and stellar Al spectra the influence of hydrogen collisions could be better estimated. The previously dened atomic model thus had to be slightly modied to t both metal-rich and metal-poor stars. ComparedwithLTEanalysesthepresentresultscompletely change the chemical enrichment scenario with (Al/Fe) now fol- lowing the trend of primary elements for all metal-poor stars. The hump of enhanced Al/Fe values for stars between 1:0 < (Fe/H) < 0:5 does not seem to be an artefact. It nearly van- ishes for the (Mg/Fe) abundance ratios. It may not necessarily have to be explained in terms of stellar nucleosynthesis because it could result from our reference to LTE abundances for Mg and Fe." @default.
- W2133921410 created "2016-06-24" @default.
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- W2133921410 date "1997-09-01" @default.
- W2133921410 modified "2023-09-26" @default.
- W2133921410 title "Aluminium in metal-poor stars." @default.
- W2133921410 hasPublicationYear "1997" @default.
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