Abstract
A programme has been under way to determine the orbital period of the symbiotic low mass X-ray binary GX 1+4. This programme aims to measure the cyclic variations of the Hα emission line feature of the optical counterpart, V2116 Oph, of this luminous X-ray pulsar. Present results indicate that the orbital period may be significantly greater than the 304 day value previously proposed. Some anomalies in the spectral characteristics of the source are discussed.
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