2012MNRAS.424.2265L

Symbiotic X-ray binaries (SyXBs) comprise a rare class of low-mass X-ray binaries. We study the Galactic SyXBs, which we consider as detached binaries composed of low-mass giants and wind-fed neutron star (NS) companions, by simulation of the interaction of a magnetized NS with its environment and utilizing a population synthesis code. We focus mainly on the parameters that influence the observational appearance of an SyXB: the donor wind velocity (v_w) and the angular momentum distribution in the shell of matter settling on to an NS. We estimate the birthrate of SyXBs as ∼ 4.1 {x} 10^–5 to ∼ 6.6 {x} 10^–6/yr and their number in the Galaxy as ∼ 100–1000. The assumed stellar wind velocity from cool giants is the input parameter that influences the model SyXB population most.

Among known SyXBs or candidate systems, 4U 1954+31 and IGR J16358-4724 in which the NSs have very long spin periods may host quasi-spherically accreting NSs. GX 1+4 has a peculiar long-term spin behaviour and it may also be a quasi-spherical wind-accreting source. We cannot identify whether there are wind-fed accretion discs in 4U 1700+24, Sct X-1, IRXS J180431.1-273932 and 2XMM J174016.0-290337. A search of CO emission lines in blazars: the low molecular gas content of BL Lac objects compared to quasars