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Abstract: The spectral distributions of Be-X-ray binaries in the Large Magellanic Cloudand Galaxy have been shown to differ significantly from the distribution ofisolated Be stars in the Galaxy. Population synthesis models can explain thisdifference in spectral distributions through substantial angular momentum lossfrom the binary system. In this work we explore the spectral distribution ofBe-X-ray binaries in the Small Magellanic Cloud SMC using highsignal-to-noise spectroscopy of a sample of 37 optical counterparts to knownX-ray pulsars. Our results show that the spectral distribution of Be-X-raybinaries in the SMC is consistent with that of the Galaxy, despite the lowermetallicity environment of the SMC. This may indicate that, although themetallicity of the SMC is conducive to the formation of a large number ofHMXBs, the spectral distribution of these systems is likely to be most stronglyinfluenced by angular momentum losses during binary evolution, which are notparticularly dependent on the local metallicity.

Autor: V.A. McBride, M.J. Coe, I. Negueruela, M.P.E. Schurch, K.E. McGowan

Fuente: https://arxiv.org/

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