The Hot Star Triplet HD 206267A
Abstract
We have observed the triple O star system HD 206267 with Chandra HETGS for the purpose of studying the properties and dynamics of the system's stellar wind. The triple system includes a 3.7 day binary which was observed once at each of the two phases of quadrature. The spectrum contains emission lines from hydrogen and helium-like oxygen, neon, and magnesium, helium-like silicon and the iron L-shell ions XVII, XVIII, and XIX. We have fit this spectrum with a combination of emission-line spectra of the individual ions at the temperatures at which the populations of the ions peak. From this fit we derive a temperature differential emission measure distribution which is cut off at temperatures above ~10 MK. All lines are very broad with HWHM velocities of ~ 1500 - 2000 km/s. The Lyman_alpha lines from O, Ne, and Mg are blue shifted and asymmetric as would be expected from shocks within a line driven wind of considerable continuum opacity. The stellar triplet revealed the main orbital velocity of 320 km/s through shifts in the X-ray lines. So far, we have not found any indications for a colliding wind in the X-ray spectrum.
- Publication:
-
High Resolution X-ray Spectroscopy with XMM-Newton and Chandra
- Pub Date:
- December 2002
- Bibcode:
- 2002hrxs.confE..49W