Astronomy and Astrophysics, volume 398, 203-211 (2003/1-4)
High-resolution X-ray spectroscopy of τ Scorpii (B0.2V) with XMM-Newton.
MEWE R., RAASSEN A.J.J., CASSINELLI J.P., VAN DER HUCHT K.A., MILLER N.A. and GUEDEL M.
Abstract (from CDS):
We report the analysis of the first high-resolution X-ray spectrum of the B0.2V star τ Scorpii obtained with the Reflection Grating Spectrometers (rgs) and the epic-mos ccd spectrometers on board XMM-Newton. The spectrum exhibits bright emission lines of the H- and He-like ions of C, N, O, Ne, Mg, and Si, as well as Fe XVII & Fe XVIII lines. Line fluxes have been determined. Simultaneous fits to the rgs and epic spectra were used to obtain four plasma temperatures, emission measures, and the overall elemental abundances. This multi-temperature fitting yielded temperatures of 1.6, 5.2, 8.2, and >20MK. These temperatures are confirmed by DEM modelling. The nitrogen lines are relatively strong: the N/O abundance ratio is about 3xsolar. No indication of a solar-type ``FIP effect'' was found for the other elements. According to the derived models the X-ray luminosity in the energy range 0.3-10keV is L_ x_=3.2x1031erg/s at a distance of 132pc. The sensitivity of the He-like forbidden and intercombination lines to a strong ultraviolet radiation field is used to derive upper limits to the radial distances at which lines of Mg XI, Ne IX, O VII, and N VI originate. The results suggest that the soft X-rays (≲8MK) originate from shocks low in the wind that are produced by the common mechanism of radiation line-driven instabilities. This is consistent with the observed emission line profiles that are much narrower (≲500km/s) than the broad lines (up to 1500km/s) observed high up in the wind of ζ Puppis. The hot (∼20-40MK) component may be explained by a model involving dense clumps embedded in a wind which sweeps past them at high relative velocity (∼1400-1700km/s). Such an interaction would produce the strong shocks required.
stars: individual: τ Scorpii - stars: coronae - stars: early-type - stars: abundances - X-rays: stars
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