Please use this identifier to cite or link to this item: https://doi.org/10.1051/0004-6361/200913724
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dc.titleThe model constraints from the observed trends for the quasi-periodic oscillation in RE J1034+396
dc.contributor.authorCzerny, B.
dc.contributor.authorLachowicz, P.
dc.contributor.authorDovčiak, M.
dc.contributor.authorKaras, V.
dc.contributor.authorPecháček, T.
dc.contributor.authorDas, T.K.
dc.date.accessioned2014-12-12T07:52:19Z
dc.date.available2014-12-12T07:52:19Z
dc.date.issued2010-12
dc.identifier.citationCzerny, B., Lachowicz, P., Dovčiak, M., Karas, V., Pecháček, T., Das, T.K. (2010-12). The model constraints from the observed trends for the quasi-periodic oscillation in RE J1034+396. Astronomy and Astrophysics 524 (5) : -. ScholarBank@NUS Repository. https://doi.org/10.1051/0004-6361/200913724
dc.identifier.issn00046361
dc.identifier.urihttp://scholarbank.nus.edu.sg/handle/10635/116637
dc.description.abstractWe analyze the time variability of the X-ray emission of RE J1034+396 - an active galactic nucleus with the first firm detection of a quasi-periodic oscillations (QPO). Based on the results of a wavelet analysis, we find a drift in the QPO central frequency. The change in the QPO frequency correlates with the change in the X-ray flux with a short time delay. The data specifically suggest a linear dependence between the QPO period and the flux, and this gives important constraints on the QPO models. In particular, it excludes explanation in terms of the orbiting hot spot model close to a black hole. Linear structures such as shocks, spiral waves, or very distant flares are favored. © 2010 ESO.
dc.sourceScopus
dc.subjectaccretion
dc.subjectaccretion disks
dc.subjectgalaxies: active
dc.subjectgalaxies: individual: RE J1034+396
dc.typeArticle
dc.contributor.departmentTEMASEK LABORATORIES
dc.description.doi10.1051/0004-6361/200913724
dc.description.sourcetitleAstronomy and Astrophysics
dc.description.volume524
dc.description.issue5
dc.description.page-
dc.description.codenAAEJA
dc.identifier.isiut000284625300015
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