Photoionization Emission Models for the Cyg X-3 X-ray Spectrum

Abstract

We present model fits to the X-ray line spectrum of the well known High Mass X-ray binary Cyg X-3. The primary observational dataset is a spectrum taken with the $Chandra$ X-ray Observatory High Energy Transmission Grating (HETG) in 2006, though we compare it to all the other observations of this source taken so far by this instrument. We show that the density must be $\ge 10^{12}$ cm${}^{-3}$ in the region responsible for most of the emission. We discuss the influence of the dust scattering halo on the broad band spectrum and we argue that dust scattering and extinction is not the most likely origin for the narrow featureseen near the Si K edge. We identify the features of a wind in the profiles of the strong resonance lines and we show that the wind is more apparent in the lines from the lighter elements. We argue that this wind is most likely associated with the companion star. We show that the intensities of most lines can be fitted, crudely, by a single component photoionized model. However, the iron K lines do not fit with this model. We show that the iron K line variability as a function of orbital phase is different from the lower energy lines, which indicates that the lines arise in physically distinct regions. We discuss the interpretation of these results in the context of what is known about the system and similar sys

arXiv commentApJ Submitted

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• Wind suppression by X-rays in Cygnus X-3
• A HaloSat Analysis of the Cygnus Superbubble
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• Spectroscopic modelling of two high-mass X-ray binaries, Cyg X--3 and 4U 1538--522
• Birthplaces of X-ray emission lines in Cygnus X-3