<?xml version="1.0" encoding="UTF-8"?><xml><records><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Mastichiadis, A.</style></author><author><style face="normal" font="default" size="100%">Oegelman, H.</style></author><author><style face="normal" font="default" size="100%">Kirk, J. G.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Spectral characteristics of the emerging X-rays from a possible pulsar in supernova 1987A.</style></title><short-title><style face="normal" font="default" size="100%">Astronomy and Astrophysics</style></short-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Astronomical Models</style></keyword><keyword><style  face="normal" font="default" size="100%">Astrophysics</style></keyword><keyword><style  face="normal" font="default" size="100%">Monte Carlo method</style></keyword><keyword><style  face="normal" font="default" size="100%">Neutron stars</style></keyword><keyword><style  face="normal" font="default" size="100%">Pulsars</style></keyword><keyword><style  face="normal" font="default" size="100%">Stellar Envelopes</style></keyword><keyword><style  face="normal" font="default" size="100%">Stellar Spectra</style></keyword><keyword><style  face="normal" font="default" size="100%">Supernova 1987a</style></keyword><keyword><style  face="normal" font="default" size="100%">X Ray Astronomy</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">1988</style></year><pub-dates><date><style  face="normal" font="default" size="100%">1988/07/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/1988A&amp;A...201L..19M</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">201</style></volume><pages><style face="normal" font="default" size="100%">L19 - L22</style></pages><isbn><style face="normal" font="default" size="100%">0004-6361</style></isbn><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">We report 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, we discuss the possibilities of observing its radiation and find 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), we do not expect pulses to be detected straightaway. Our conclusions are based on a simple homogeneous model for the envelope and do not depend on whether or not ^56^Co 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 our results.</style></abstract></record></records></xml>