Tracking The Orbital And Super-orbital Periods Of SMC X-1

Astronomy and Astrophysics – Astronomy

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Scientific paper

SMC X-1 is a partially wind-fed, high mass X-ray binary system with an X-ray pulsar primary. Similar to Her X-1, the system exhibits a `super-orbital' periodicity. Such super-orbital periods have been attributed to warped, precessing accretion disks (see Pringle 1996; Maloney, Begelman, and Pringle 1996; Maloney and Begelman 1997; Maloney, Begelman, and Nowak 1998; Ogilvie and Dubus 2001).
In contrast to Her X-1, the SMC X-1 super-orbital period is extremely unsteady - varying between 35-70 days. This has been attributed to the presence of multiple "warp modes" in the accretion disk (e.g., Clarkson et al. 2003). Here we instead explore the hypothesis of a single warp mode with a varying period. We use the RXTE-ASM data to study the period variations, and we present a "two dimensional" epoch fold of the data on both the orbital and super-orbital periods.
We discuss possible correlations between the system flux, the super-orbital period duration, and the pulsar spin-up/spin-down. We make analogies to similar, albeit far less dramatic, behavior seen in Her X-1.

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