Show simple item record

dc.contributor.authorErkut, M. Hakan
dc.date.accessioned2018-08-01T13:03:46Z
dc.date.available2018-08-01T13:03:46Z
dc.date.issued2011
dc.identifier.isbn978-0-7354-0939-2
dc.identifier.issn0094-243X
dc.identifier.urihttps://doi.org/10.1063/1.3629493
dc.identifier.urihttps://hdl.handle.net/11413/2473
dc.description.abstractThe kHz QPOs observed in a neutron star low mass X-ray binary are likely to be produced in the innermost regions of accretion disk around the neutron star. The rotational dynamics of the inner disk can be characterized by the presence of either sub-Keplerian or super-Keplerian accretion flow depending on the relative fastness of the neutron spin as compared to the Keplerian frequency at the inner disk radius. Within the magnetosphere-disk interaction model, the frequency difference between the two kHz QPOs observed in a given source can be estimated to be slightly higher than or nearly around the neutron star spin frequency if the neutron star is a slow rotator and less than the stellar spin frequency if the neutron star is a fast rotator.tr_TR
dc.language.isoen_UStr_TR
dc.publisherAmer Inst Physics, 2 Huntington Quadrangle, Ste 1No1, Melville, Ny 11747-4501 USAtr_TR
dc.relationAstrophysics of Neutron Stars 2010: a Conference in Honor of M. Ali Alpartr_TR
dc.subjectAccretion and accretion diskstr_TR
dc.subjectOscillationstr_TR
dc.subjectNeutron starstr_TR
dc.subjectX-ray binariestr_TR
dc.subjectOscillationstr_TR
dc.titleHigh-Frequency QPOs as a Product of Inner Disk Dynamics around Neutron Starstr_TR
dc.typeArticletr_TR
dc.identifier.wos302936600018
dc.identifier.wos302936600018en
dc.identifier.scopus2-s2.0-80053350847
dc.identifier.scopus2-s2.0-80053350847en


Files in this item

FilesSizeFormatView

There are no files associated with this item.

This item appears in the following Collection(s)

Show simple item record