@article {2000ApJ...545L.135S,
	title = {{X-Ray Line Emission from the Hot Stellar Wind of {\th}etas}$^{1}$ Orionis C}},
	journal = {\apjl},
	volume = {545},
	year = {2000},
	note = {n/a},
	month = {dec},
	pages = {L135-L139},
	abstract = {{We present a first emission-line analysis of a high-resolution X-ray spectrum of the stellar wind of {\th}etas}$^{1}$ Ori C obtained with the High-Energy Transmission Grating Spectrometer on board the Chandra X-Ray Observatory. The spectra are resolved into a large number of emission lines from H- and He-like O, Ne, Mg, Si, S, Ar, and Fe ions. The He-like Fe XXV and Li-like Fe XXIV appear quite strong, indicating very hot emitting regions. From H/He flux ratios as well as from Fe He/Li emission measure ratios, we deduce temperatures ranging from 0.5 to 6.1{\times}10$^{7}$ K. The He triplets are very sensitive to density as well. At these temperatures the relative strengths of the intercombination and forbidden lines indicate electron densities well above 10$^{12}$ cm$^{-3}$. The lines appear significantly broadened, from which we deduce 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 the X-ray emission could originate in dense and hot regions with a characteristic size of less then 4{\times}10$^{10}$ cm. }
},
	doi = {10.1086/317891},
	author = {{Schulz}, N.~S. and {Canizares}, C.~R. and {Huenemoerder}, D. and {Lee}, J.~C.}
}
