Cylotron line models for the X-ray pulsar A0535+26
  The spectrum of the transient X-ray binary pulsar A0535+26 obtained by OSSE in February 1994 shows an absorption feature at 110 keV but does not confirm a feature at around 55 keV, as previously reported by other instruments. If the 110 keV feature is due to cyclotron scattering at the first harmonic, then the magnetic field required is about $10^{13}$ Gauss, the highest observed in an X-ray pulsar. Conversely, if this strong feature is a second harmonic and the line formation process is such that an extremely weak fundamental results at $\simeq$ 55 keV, the estimate of the field strength is halved. We present results of detailed cyclotron line transfer models from two source geometries to explore the theoretical contraints on the line shapes in this source. It is found that while a fundamental harmonic line at $\sim$ 55 keV may be partially filled-in by angle redistribution in cylindrical geometries, the required viewing angles give a second harmonic line shape inconsistent with the observation. Interpretation of the feature at 110 keV as a first harmonic seen at small angles to the field yields more consistent line shapes. 
R. A. Araya (Johns Hopkins Univ.) and A. K. Harding (NASA Goddard)