Superorbital periods of Be/X-ray binaries driven by stellar spin precession

Abstract

Superorbital periods are observed in the optical light curves of many Be/X-ray binaries yet their origin has remained somewhat elusive. We suggest that precession of the spin axis of the Be star can drive superorbital periods, particularly for short orbital period binaries. We consider the short orbital period ($P_{\mathrm{orb}}=16.6\mathrm{day}$) and highly eccentric ($e_{\mathrm{b}}=0.72$) Be/X-ray binary A0538-66 that has a superorbital period of $421\mathrm{day}$. First we show that the spin axis precession timescale is about twice the observed superorbital period. Then, with hydrodynamic simulations we show that the Be star decretion disc can remain locked to the equator of the precessing Be star. At each periastron passage of the neutron star, material is accreted into a disc around the neutron star. The neutron star disc nodally precesses on the same timescale as the Be star disc and therefore both discs can contribute to the observed superorbital period. For wider and less eccentric binary systems, the Be star disc can have a larger radial extent and more complex behaviour is expected as a result of disc warping and breaking.

Accepted for publication in MNRAS Letters

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