A 2 h periodic variation in the low-mass X-ray binary Ser X-1

Cornelisse, R.; Casares, J.; Charles, P. A.; Steeghs, D.
Bibliographical reference

Monthly Notices of the Royal Astronomical Society, Volume 432, Issue 2, p.1361-1366

Advertised on:
Spectroscopy of the low-mass X-ray binary Ser X-1 using the Gran Telescopio Canarias have revealed a ≃2 h periodic variability that is present in the three strongest emission lines. We tentatively interpret this variability as due to orbital motion, making it the first indication of the orbital period of Ser X-1. Together with the fact that the emission lines are remarkably narrow, but still resolved, we show that a main-sequence K dwarf together with a canonical 1.4 M⊙ neutron star gives a good description of the system. In this scenario, the most likely place for the emission lines to arise is the accretion disc, instead of a localized region in the binary (such as the irradiated surface or the stream-impact point), and their narrowness is due instead to the low inclination (≤10°) of Ser X-1.
Related projects
Black hole in outburst
Nature and Evolution of X-Ray Binaries

Accreting black-holes and neutron stars in X-ray binaries provide an ideal laboratory for exploring the physics of compact objects, yielding not only confirmation of the existence of stellar mass black holes via dynamical mass measurements, but also the best opportunity for probing high-gravity environments and the physics of accretion; the most

Muñoz Darias