SIMBAD references

Context. Obtaining precise stellar and wind properties and abundance patterns of massive stars is crucial to understanding their nature and interactions with their environments, as well as to constrain their evolutionary paths and end-products.
Aims. To enable higher versatility and precision of the complete ultraviolet (UV) to optical range, we improve our high-performance, unified, NLTE atmosphere and spectrum synthesis codeFASTWIND. Moreover, we aim to obtain an advanced description of X-ray emission from wind-embedded shocks, consistent with alternative modeling approaches.
Methods. We include a detailed comoving frame radiative transfer for the essential frequency range, but still apply methods that enable low turnaround times. We compare the results of our updated computations with those from the alternative codeCMFGEN, and our previousFASTWIND version, for a representative model grid.
Results. In most cases, our new results agree excellently with those fromCMFGEN, both regarding the total radiative acceleration, strategic optical lines, and the UV-range. Moderate differences concern HeIIλλ4200-4541 and NVλλ4603-4619. The agreement regarding NIIIλλ4634-4640-4642 has improved, though there are still certain discrepancies, mostly related to line overlap effects in the extreme ultraviolet, depending on abundances and micro-turbulence. In the UV range of our coolest models, we find differences in the predicted depression of the pseudo-continuum, which is most pronounced around Lyα. This depression is larger inCMFGEN, and related to different FeIV atomic data. The comparison between our new and previousFASTWIND version reveals an almost perfect agreement, except again for NVλλ4603-4619. Using an improved, depth-dependent description for the filling factors of hot, X-ray emitting material, we confirm previous analytic scaling relations with our numerical models.
Conclusions. We warn against uncritically relying on transitions, which are strongly affected by direct or indirect line-overlap effects. The predicted UV-continuum depression for the coolest grid-models needs to be checked, both observationally, and regarding the underlying atomic data. Wind lines from "super-ionized" ions such as OVI can, in principle, be used to constrain the distribution of wind-embedded shocks. The newFASTWIND version v11 is now ready to be used.