X-ray line emission from the hot stellar wind of theta(1) Orionis C

We present a first emission-line analysis of a high-resolution X-ray spectr um of the stellar wind of theta (1) Ori C obtained with the High-Energy Tra nsmission Grating Spectrometer on board the Chandra X-Ray Observatory. The spectra are resolved into a large number of emission lines from H- and He-l ike O, Ne, Mg, Si, S, Ar, and Fe ions. The He-like Fe xxv and Li-like Fe xx iv appear quite strong, indicating very hot emitting regions. From H/He flu x ratios as well as from Fe He/Li emission measure ratios, we deduce temper atures ranging from 0.5 to 6.1 x 10(7) K. The He triplets are very sensitiv e to density as well. At these temperatures the relative strengths of the i ntercombination and forbidden lines indicate electron densities well above 10(12) cm(-3). The lines appear significantly broadened, from which we dedu ce a mean velocity of 770 km s(-1) with a spread between 400 and 2000 km s( -1). Along with results of the deduced emission measure, we conclude that t he X-ray emission could originate in dense and hot regions with a character istic size of less then 4 x 10(10) cm.