X-rays from a possible pulsar in supernova 1987A

The author reports on Monte-Carlo calculations of the emergence of X- and γ-rays from the envelope of the supernova 1987A. Assuming that there exists an X-ray emitting pulsar at the centre, he discusses the possibilities of observing its radiation and finds that if the pulsar is about as luminous as the present-day Crab, it may be possible to detect the breakout at ≡ 20 months. The pulsar should emerge first in the 6 - 16 keV band covered by GINGA. About six months later it would appear in the 20 - 45 keV band of MIR-HEXE. Because the optical depth of the envelope at breakout is still substantial (≡4), the author does not expect pulses to be detected straightaway. His conclusions are based on a simple homogeneous model for the envelope and do not depend on whether or not ⁵⁶Co is mixed into the outer layers. The time at which a pulsar of higher luminosity would emerge can be obtained from a simple scaling of the results.