2003MNRAS.341.1231T

We present time-resolved spectroscopy acquired during two epochs (spaced apart by ∼15 d) of the eclipsing low-mass X-ray binary AC211/X2127+119 in the globular cluster M15. The spectra show variations in the Heiiλ4686 emission line not only modulated on the orbital period, but also on time-scales of a few days. During the first epoch of observation, the emission line shows a strong S -wave superimposed on the average double-peaked profile. The line exhibits no evidence of rotational disturbance at the orbital phases when the eclipse is observed in the optical continuum. During the second epoch, no double-peak or S -wave component is present. The Hei absorption lines detected by other authors are not present in our spectra. A Doppler image of Heiiλ4686 for the first epoch supports the presence of the accretion disc. No hotspot is detected, although enhanced emission at V_X=30 km.s^–1, V_Y=160 km.s^–1 is observed. We discuss the implications of this emission in the context of an X-ray heated donor star, in which case a high mass ratio and neutron star primary are implied. Finally, we speculate on the possibility of a misaligned secondary star in AC211.