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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/5347
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dc.contributor.authorSingh, N.S.-
dc.contributor.authorNaik, S.-
dc.contributor.authorPaul, Biswajit-
dc.contributor.authorAgrawal, P.C.-
dc.contributor.authorRao, A.R.-
dc.contributor.authorSingh, K.Y.-
dc.date.accessioned2012-12-14T09:28:40Z-
dc.date.available2012-12-14T09:28:40Z-
dc.date.issued2002-09-
dc.identifier.citationAstronomy and Astrophysics, 2002, Vol.392, p161-167en
dc.identifier.issn0004-6361-
dc.identifier.issn1432-0746(Online)-
dc.identifier.urihttp://hdl.handle.net/2289/5347-
dc.descriptionRestricted Access.en
dc.description.abstractThe nonlinear nature of the binary ephemeris of Cygnus X-3 indicates either a change in the orbital period or an apsidal motion of the orbit. We have made extended observations of Cygnus X-3 with the Pointed Proportional Counters (PPCs) of the Indian X-ray Astronomy Experiment (IXAE) during 1999 July 3−13 and October 11−14. Using the data from these observations and the archival data from ROSAT, ASCA, BeppoSAX and RXTE, we have extended the database for this source. Adding these new arrival time measurements to the published results, we make a comparison between the various possibilities, (a) orbital decay due to mass loss from the system, (b) mass transfer between the stars, and (c) apsidal motion of the orbit due to gravitational interaction between the two components. The orbital decay due to mass loss from the companion star seems to be the most probable scenarioen
dc.language.isoenen
dc.publisherSpringer Verlagen
dc.relation.urihttp://adsabs.harvard.edu/abs/2002A%26A...392..161Sen
dc.relation.urihttp://arxiv.org/abs/astro-ph/0206134en
dc.relation.urihttp://dx.doi.org/10.1051/0004-6361:20020923en
dc.rights2002, Springer Verlagen
dc.subjectstarsen
dc.subjectbinariesen
dc.subjectCygnus X-3en
dc.subjectWolf-Rayeten
dc.subjectX-rayen
dc.titleNew measurements of orbital period change in Cygnus X-3en
dc.typeArticleen
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