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• W3100929627 endingPage "852" @default.
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• W3100929627 abstract "<i>Aims. <i/>We investigate the stellar and wind properties of a sample of late-type O dwarfs. Previous analyses of such stars have found very low mass-loss rates; rates much lower than predicted by theory (the weak wind problem).<i>Methods. <i/>Far-UV to optical spectra of five Galactic O stars were analyzed: HD 216898 (O9IV/O8.5V), HD 326329 (O9V), HD 66788 (O8V/O9V), <i>ζ<i/> Oph (O9.5Vnn), and HD 216532 (O8.5V((n))). We used a grid of TLUSTY models to obtain effective temperatures, gravities, rotational velocities, and to identify wind lines. Wind parameters for each object were obtained using expanding atmosphere models calculated with the CMFGEN code.<i>Results. <i/>The spectra of our sample have primarily a photospheric origin. A weak wind signature is seen in C iv 1548, 1551, from which mass-loss rates consistent with previous CMFGEN results for O8-O9V stars were derived ( yr<sup>-1<sup/>). A discrepancy of roughly two orders of magnitude is found between these mass-loss rates and the values predicted by theory (), confirming a breakdown or a steepening of the modified wind momentum-luminosity relation at log . We have estimated the carbon abundance for the stars of our sample and concluded that its value cannot be reduced to sufficiently small values to solve the <i>weak wind problem<i/>. Upper limits on were established for all objects using lines of different ions: P v 1118, 1128, C iii , N v 1239, 1243, Si iv 1394, 1403, and N iv <i>λ<i/>1718. All the values obtained are in disagreement with theoretical predictions, bringing support to the reality of <i>weak winds<i/>. Together with C iv 1548, 1551, the use of N v 1239, 1243 results in the lowest mass-loss rates: the upper limits indicate that must be <i>less<i/> than about -1.0 dex . Upper mass-loss rate limits obtained for other transitions are also low: they indicate that must be <i>less<i/> than about (-0.5 <i>±<i/> 0.2) dex . We studied the behavior of the H<i>α<i/> line with different mass-loss rates. For two stars, only models with very low 's provide the best fit to the UV and optical spectra. We also explored ways to fit the observed spectra with the theoretical mass-loss rates. By using large amounts of X-rays, we could reduce the predicted wind emission to the observed levels. However, unrealistic X-ray luminosities had to be used (log ). The validity of the models used in our analyses is discussed." @default.
• W3100929627 created "2020-11-23" @default.
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• W3100929627 date "2009-03-19" @default.
• W3100929627 modified "2023-10-04" @default.
• W3100929627 title "Analysis of Galactic late-type O dwarfs: more constraints on the weak wind problem" @default.
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• W3100929627 doi "https://doi.org/10.1051/0004-6361/200811289" @default.
• W3100929627 hasPublicationYear "2009" @default.
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