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INTEGRAL Observations of OAO 1657-415: Gamma-Ray Tomography of a B Super Giant

Denis M., Bulik T., Marcinkowski R.

Acta Astronomica

2010

Vol. 60, No. 1

75--82

OAO 1657-415 is an accreting pulsar in an eclipsing binary system. We analyzed the INTEGRAL core program observations of this object and obtained the eclipse light curve in the soft gamma-ray band between 15 keV and 40 keV. We note that the gamma rays from the pulsar allow to probe the density profile of the outer layers of the B super giant companion. We find that the density profile of the outer layer can be described by a power law with the index α=8.5. We also note that the fit hints toward smaller inclinations of the system within the allowed range 60°

The Effect of e+e- Pair Production on Gamma-Ray Luminosities of Pulsars

Dyks J.

Acta Astronomica

1998

Vol. 48, No. 2

355--372

We present details of a modified phenomenological polar cap model of γ-ray emission from pulsars, introduced recently by Rudak and Dyks (1998). The model attributes observed γ-rays mostly to electron-positron pairs created in magnetospheres by high energy curvature photons emitted by primary electrons. We show how the basic ingredient of the model - the number of created e± pairs - depends on the pulsar period, and the magnetic field, for two different prescriptions for the energy of the primaries, and how it affects predictions for the γ-ray luminosity. The model has been successfully applied to the results of the Compton Gamma Ray Observatory (CGRO) observations.