Abstract
We report Ariel V(SSI) observations of three X-ray pulsars A0535+26, 2S1145-619 and GX301-2 (2S1223-624). These sources exhibit X-ray outbursts which appear, on the basis of observations extending over ∿ 5 years, to have recurrence periods of 110 days, 187.5 days and 41.4 days respectively. If these periods are orbital in origin, the observed X-ray modulation may be explained in terms of an appreciable orbital eccentricity giving rise to time variable accretion. (In the case of GX301-2 published pulse timing data already provide independent evidence for a 41.4 day orbital period and an eccentricity e ≈ 0.4). The optical counterparts are all early-type stars; A0535+26 and 2S1145-619 are identified with Be main sequence stars and GX301-2 with a B2 supergiant which also shows an emission line spectrum. The implications of the observations in relation to possible mass transfer mechanisms in such systems are discussed.
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© 1981 Springer Science+Business Media Dordrecht
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Warwick, R.S., Watson, M.G., Sims, M.R. (1981). Periodic X-Ray Outbursts from A0535+26, 2S1145-619 and GX301-2. In: Andresen, R.D. (eds) X-Ray Astronomy. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-9949-3_71
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DOI: https://doi.org/10.1007/978-94-010-9949-3_71
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