Computer Science
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002hrxs.confe..32r&link_type=abstract
High Resolution X-ray Spectroscopy with XMM-Newton and Chandra, Proceedings of the international workshop held at the Mullard Sp
Computer Science
Scientific paper
The spectra of the B0.2V star Tau Scorpii, observed with RGS and EPIC-MOS on board XMM-Newton, are simultaneously fitted to obtain self-consistent temperatures, emission measures, and elemental abundances. The nitrogen lines are relatively very strong: the N/O abundance ratio is about 3 times solar. Multi-temperature fitting yields 4 components at temperatures of 1.6, 5.2, 8.2, and >~ 20 MK which are confirmed by DEM modeling. The X-ray luminosity (0.3-10 keV) is 3.2e31 erg/s at d=132 pc. The sensitivity of the He-like forbidden and intercombination lines to a strong UV stellar radiation field yields upper limits to the radial distances at which the He-like lines of Mg, Ne, O, and N originate. The results suggest that the soft X-rays (<~ 8 MK) originate from shocks low in the wind produced by the common mechanism of radiation line-driven instabilities. This is consistent with the observed emission line profiles that are much narrower (<~ 500 km/s) than the broad lines (up to 1500 km/s) observed high up in the wind of Zeta Puppis. The hot (~ 20-40 MK) component may be explained by a model involving dense clumps embedded in a wind which is approaching at high relative velocity (~ 1400-1700 km/s) and the interaction produces strong shocks.
Cassinelli Joe P.
Guedel Manuel
Mewe Rolf
Miller Nancy A.
Raassen Ton
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