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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/5538
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dc.contributor.authorNair, Sachindra-
dc.contributor.authorMaitra, Chandreyee-
dc.contributor.authorJaisawal, Gaurava K.-
dc.contributor.authorPaul, Biswajit-
dc.date.accessioned2013-04-15T09:22:16Z-
dc.date.available2013-04-15T09:22:16Z-
dc.date.issued2013-02-
dc.identifier.citationThe Astrophysical Journal, 2013, Vol.764, p158en
dc.identifier.issn0004-637X-
dc.identifier.issn1538-4357 (Online)-
dc.identifier.urihttp://hdl.handle.net/2289/5538-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations) Articles older than 2 years are open to all at the journal siteen
dc.description.abstractWe present results from a study of broadband timing and spectral properties of EXO 2030+375 using a Suzaku observation. Pulsations with a period of 41.41 s and strong energy-dependent pulse profiles were clearly detected up to 100 keV. Narrow dips are seen in the profiles up to ~70 keV. The presence of prominent dips at several phases in the profiles up to such high energy ranges was not seen before. At higher energies, these dips gradually disappeared and the profile appeared to be single-peaked. The 1.0-200.0 keV broadband spectrum is found to be well described by a partial covering high-energy cutoff power-law model. Several low-energy emission lines are also detected in the pulsar spectrum. We fitted the spectrum using neutral as well as partially ionized absorbers along with the above continuum model yielding similar parameter values. The partial covering with a partially ionized absorber resulted in a marginally better fit. The spectral fitting did not require any cyclotron feature in the best-fit model. To investigate the changes in spectral parameters at dips, we carried out pulse-phase-resolved spectroscopy. During the dips, the value of the additional column density was estimated to be high compared to other pulse phases. While using a partially ionized absorber, the value of the ionization parameter is also higher at the dips. This may be the reason for the presence of dips up to higher energies. No other spectral parameters show any systematic variation with pulse phases of the pulsar.en
dc.language.isoenen
dc.publisherIOP Sciences for The American Astronomical Society.en
dc.relation.urihttp://adsabs.harvard.edu/abs/2013ApJ...764..158Nen
dc.relation.urihttp://arxiv.org/abs/1301.1112en
dc.relation.urihttp://dx.doi.org/10.1088/0004-637X/764/2/158en
dc.rights2013, The American Astronomical Society.en
dc.subjectindividual (EXO 2030+375)en
dc.subjectstars: neutronen
dc.subjectX-rays: starsen
dc.titleTiming and Spectral properties of Be/X-ray pulsar EXO 2030+375 during a Type I outbursten
dc.typeArticleen
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