X-ray diagnostics of chemical composition of the accretion disk and donor star in ultra-compact X-ray binaries

TL;DR

This paper investigates how non-solar chemical compositions in ultra-compact X-ray binaries affect their X-ray spectra, especially the iron fluorescence lines, enabling the identification of donor star types through spectral analysis.

Contribution

It demonstrates that anomalous C/O abundances significantly alter iron line strengths, providing a new method to determine donor star composition via X-ray spectroscopy.

Findings

Iron Kα line is suppressed by oxygen screening in C/O-rich material.

Iron line strength depends on luminosity, recovering at higher luminosities.

He-rich donors do not significantly affect iron line strength.

Abstract

Non-solar composition of the donor star in ultra-compact X-ray binaries may have a pronounced effect on the fluorescent lines appearing in their spectra due to reprocessing of primary radiation by the accretion disk and the white dwarf surface. We show that the most dramatic and easily observable consequence of the anomalous C/O abundance, is the significant, by more than an order of magnitude, attenuation of the Ka line of iron. It is caused by screening of the presence of iron by oxygen - in the C/O dominated material the main interaction process for a E ~ 7keV photon is absorption by oxygen rather than by iron, contrary to the solar composition case. Ionization of oxygen at high mass accretion rates adds a luminosity dependence to this behavior - the iron line is significantly suppressed only at low luminosity, log(LX) less than 37-37.5, and should recover its nominal strength at higher luminosity. The increase of the EW of the Ka lines of carbon and oxygen, on the other hand, saturates at rather moderate values. Screening by He is less important, due to its low ionization threshold and because in the accretion disk it is mostly ionized. Consequently, in the case of the He-rich donor, the iron line strength remains close to its nominal value, determined by the iron abundance in the accretion disk. This opens the possibility of constraining the nature of donor stars in UCXBs by means of X-ray spectroscopy with moderate energy resolution.