Photoionization Emission Models for the Cyg X-3 X-ray Spectrum. (arXiv:1902.05589v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kallman_T/0/1/0/all/0/1">T. Kallman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McCollough_M/0/1/0/all/0/1">M. McCollough</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koljonen_K/0/1/0/all/0/1">K. Koljonen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liedahl_D/0/1/0/all/0/1">D. Liedahl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miller_J/0/1/0/all/0/1">J. Miller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paerels_F/0/1/0/all/0/1">F. Paerels</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pooley_G/0/1/0/all/0/1">G. Pooley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sako_M/0/1/0/all/0/1">M. Sako</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schulz_N/0/1/0/all/0/1">N. Schulz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Trushkin_S/0/1/0/all/0/1">S. Trushkin</a>
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 $geq 10^{12}$
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
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 $geq 10^{12}$
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
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