FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W3100106785> ?p ?o ?g. }

• W3100106785 abstract "Context. Nitrogen is a key element for testing the impact of rotational mixing on evolutionary models of massive stars. Recent studies of the nitrogen surface abundance in B-type stars within the VLT-FLAMES survey of massive stars have challenged part of the corresponding predictions. To obtain a more complete picture of massive star evolution, and to allow for additional constraints, these studies need to be extended to O-stars.Aims. This is the second paper in a series aiming at the analysis of nitrogen abundances in O-type stars, to establish tighter constraints on the early evolution of massive stars. In this paper, we investigate the N ivλ 4058 emission line formation, provide nitrogen abundances for a substantial O-star sample in the Large Magellanic Cloud, and compare our (preliminary) findings with recent predictions from stellar evolutionary models.Methods. Stellar and wind parameters of our sample stars were determined by line profile fitting of hydrogen, helium and nitrogen lines, exploiting the corresponding ionization equilibria. Synthetic spectra were calculated by means of the NLTE atmosphere/spectrum synthesis code fastwind, using a new nitrogen model atom. We derived nitrogen abundances for 20 O- and 5 B-stars by analyzing all nitrogen lines (from different ionization stages) present in the available optical spectra.Results. The dominating process responsible for emission at N ivλ 4058 in O-stars is the strong depopulation of the lower level of the transition, which increases as a function of Ṁ . Unlike the N iii triplet emission, resonance lines do not play a role for typical mass-loss rates and below. We find (almost) no problem in fitting the nitrogen lines, in particular the “f” features. Only for some objects, where lines from N iii/N iv/N v are visible in parallel, we need to opt for a compromise solution. For five objects in the early B-/late O-star domain that have been previously analyzed by different methods and model atmospheres, we derive consistent nitrogen abundances. The bulk of our sample O-stars seems to be strongly nitrogen-enriched, and a clear correlation of nitrogen and helium enrichment is found. By comparing the nitrogen abundances as a function of v    sin   i (“Hunter-plot”) with tailored evolutionary calculations, we identify a considerable number of highly enriched objects at low rotation. Conclusions. Our findings seem to support the basic outcome of previous B-star studies within the VLT-FLAMES survey. Owing to the low initial abundance, the detection of strong nitrogen enrichment in the bulk of O-stars indicates that efficient mixing takes place already during the very early phases of stellar evolution of LMC O-stars. For tighter constraints, however, upcoming results from the VLT-FLAMES Tarantula survey need to be waited for, which will comprise a much higher number of O-stars that will be analyzed based on similar methods as presented here." @default.
• W3100106785 created "2020-11-23" @default.
• W3100106785 creator A5002227853 @default.
• W3100106785 creator A5016298202 @default.
• W3100106785 creator A5021030288 @default.
• W3100106785 creator A5035958223 @default.
• W3100106785 date "2012-01-01" @default.
• W3100106785 modified "2023-09-23" @default.
• W3100106785 title "Nitrogen line spectroscopy of O-stars - II. Surface nitrogen abundances for O-stars in the Large Magellanic Cloud" @default.
• W3100106785 cites W1495978751 @default.
• W3100106785 cites W1530279911 @default.
• W3100106785 cites W1559667750 @default.
• W3100106785 cites W1659875532 @default.
• W3100106785 cites W1839232526 @default.
• W3100106785 cites W1946166908 @default.
• W3100106785 cites W1975422846 @default.
• W3100106785 cites W1977382329 @default.
• W3100106785 cites W1983806448 @default.
• W3100106785 cites W1984745062 @default.
• W3100106785 cites W1985422339 @default.
• W3100106785 cites W1986287522 @default.
• W3100106785 cites W1987076109 @default.
• W3100106785 cites W1987079650 @default.
• W3100106785 cites W1990776584 @default.
• W3100106785 cites W1993917195 @default.
• W3100106785 cites W2000771032 @default.
• W3100106785 cites W2002175961 @default.
• W3100106785 cites W2005178129 @default.
• W3100106785 cites W2006665080 @default.
• W3100106785 cites W2007906377 @default.
• W3100106785 cites W2010238408 @default.
• W3100106785 cites W2019244016 @default.
• W3100106785 cites W2019613714 @default.
• W3100106785 cites W2021733452 @default.
• W3100106785 cites W2023891552 @default.
• W3100106785 cites W2024840617 @default.
• W3100106785 cites W2024909325 @default.
• W3100106785 cites W2025807334 @default.
• W3100106785 cites W2027386627 @default.
• W3100106785 cites W2033729312 @default.
• W3100106785 cites W2036892734 @default.
• W3100106785 cites W2037338859 @default.
• W3100106785 cites W2043792386 @default.
• W3100106785 cites W2044155210 @default.
• W3100106785 cites W2049117680 @default.
• W3100106785 cites W2051104728 @default.
• W3100106785 cites W2062150455 @default.
• W3100106785 cites W2074309830 @default.
• W3100106785 cites W2081430203 @default.
• W3100106785 cites W2082254641 @default.
• W3100106785 cites W2082361137 @default.
• W3100106785 cites W2088204054 @default.
• W3100106785 cites W2092881910 @default.
• W3100106785 cites W2099442838 @default.
• W3100106785 cites W2100902642 @default.
• W3100106785 cites W2102245373 @default.
• W3100106785 cites W2113865096 @default.
• W3100106785 cites W2114574183 @default.
• W3100106785 cites W2116428272 @default.
• W3100106785 cites W2117576477 @default.
• W3100106785 cites W2122448554 @default.
• W3100106785 cites W2123423036 @default.
• W3100106785 cites W2125254020 @default.
• W3100106785 cites W2147248999 @default.
• W3100106785 cites W2163575963 @default.
• W3100106785 cites W2168939637 @default.
• W3100106785 cites W2169635684 @default.
• W3100106785 cites W2493548435 @default.
• W3100106785 cites W2610220141 @default.
• W3100106785 cites W2613831827 @default.
• W3100106785 cites W3025918851 @default.
• W3100106785 cites W3047370027 @default.
• W3100106785 cites W3098546041 @default.
• W3100106785 cites W3098654788 @default.
• W3100106785 cites W3099307424 @default.
• W3100106785 cites W3102294516 @default.
• W3100106785 cites W3102808992 @default.
• W3100106785 cites W3105744483 @default.
• W3100106785 cites W3122200469 @default.
• W3100106785 cites W3124400177 @default.
• W3100106785 cites W93867531 @default.
• W3100106785 cites W3021048390 @default.
• W3100106785 hasPublicationYear "2012" @default.
• W3100106785 type Work @default.
• W3100106785 sameAs 3100106785 @default.
• W3100106785 citedByCount "38" @default.
• W3100106785 countsByYear W31001067852012 @default.
• W3100106785 countsByYear W31001067852013 @default.
• W3100106785 countsByYear W31001067852014 @default.
• W3100106785 countsByYear W31001067852015 @default.
• W3100106785 countsByYear W31001067852016 @default.
• W3100106785 countsByYear W31001067852017 @default.
• W3100106785 countsByYear W31001067852018 @default.
• W3100106785 countsByYear W31001067852019 @default.
• W3100106785 countsByYear W31001067852020 @default.
• W3100106785 crossrefType "journal-article" @default.
• W3100106785 hasAuthorship W3100106785A5002227853 @default.
• W3100106785 hasAuthorship W3100106785A5016298202 @default.
• W3100106785 hasAuthorship W3100106785A5021030288 @default.
• W3100106785 hasAuthorship W3100106785A5035958223 @default.

• next