<?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%">Hermsen, W.</style></author><author><style face="normal" font="default" size="100%">Bennett, K.</style></author><author><style face="normal" font="default" size="100%">Bloemen, J. B. G. M.</style></author><author><style face="normal" font="default" size="100%">Buccheri, R.</style></author><author><style face="normal" font="default" size="100%">Jansen, F. A.</style></author><author><style face="normal" font="default" size="100%">Mastichiadis, A.</style></author><author><style face="normal" font="default" size="100%">Mayer-Hasselwander, H. A.</style></author><author><style face="normal" font="default" size="100%">Özel, M. E.</style></author><author><style face="normal" font="default" size="100%">Pollock, A. M. T.</style></author><author><style face="normal" font="default" size="100%">Strong, A. W.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">High-energy gamma-ray and hard X-ray observations of CYG X-3.</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%">Absorption Spectra</style></keyword><keyword><style  face="normal" font="default" size="100%">Astrophysics</style></keyword><keyword><style  face="normal" font="default" size="100%">Cos-B Satellite</style></keyword><keyword><style  face="normal" font="default" size="100%">Gamma Ray Astronomy</style></keyword><keyword><style  face="normal" font="default" size="100%">Spectrum Analysis</style></keyword><keyword><style  face="normal" font="default" size="100%">Stellar Spectra</style></keyword><keyword><style  face="normal" font="default" size="100%">X Ray Astronomy</style></keyword><keyword><style  face="normal" font="default" size="100%">X Ray Binaries</style></keyword><keyword><style  face="normal" font="default" size="100%">X Ray Spectra</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">1987</style></year><pub-dates><date><style  face="normal" font="default" size="100%">1987/03/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/1987A&amp;A...175..141H</style></url></web-urls></urls><volume><style face="normal" font="default" size="100%">175</style></volume><pages><style face="normal" font="default" size="100%">141 - 150</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%">High-energy (70 MeV &amp;lt; E &amp;lt; 5 GeV) gamma-ray observations of Cyg X-3 by the ESA satellite COS-B and hard X-ray (14 keV &amp;lt; E &amp;lt; 140 keV) observations by the Leiden-MIT balloon experiment, Leimit, are presented. A comparison with, and a study of earlier results over the 14 decades in energy from 1 keV up to ≡10&lt;SUP&gt;17&lt;/SUP&gt;eV indicates that the strong variability of Cyg X-3 over more than one order of magnitude at energies below 20 keV does not exhibit itself in the data collected at hard X-ray energies, and the power emitted per decade of energy reaches a minimum in the MeV-GeV region. If the primary gamma-rays up to 10&lt;SUP&gt;15&lt;/SUP&gt;eV originate close to the central source, absorption by the keV X-rays in the Cyg X-3 binary system could explain the latter phenomenon.</style></abstract></record></records></xml>