Soft X-ray emission lines in the X-ray binary Swift J1858.6-0814 observed with XMM-Newton-RGS: disc atmosphere or wind?
arXiv:2007.14407 · doi:10.1093/mnras/staa2258
Abstract
We find soft X-ray emission lines from the X-ray binary Swift J1858.6-0814 in data from XMM-Newton-RGS: N VII, O VII and O VIII, as well as notable residuals short of a detection at Ne IX and other higher ionisation transitions. These could be associated with the disc atmosphere, as in accretion disc corona sources, or with a wind, as has been detected in Swift J1858.6-0814 in emission lines at optical wavelengths. Indeed, the N VII line is redshifted, consistent with being the emitting component of a P-Cygni profile. We find that the emitting plasma has an ionisation parameter and a density cm. From this, we infer that the emitting plasma must be within cm of the ionising source, for a neutron star, and from the line width that it is at least away ( cm). We compare this with known classes of emission line regions in other X-ray binaries and active galactic nuclei.
10 pages, 7 figures, MNRAS accepted
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- X-ray Iron absorption line in Swift J1858.6-0814