The correlations and anticorrelations in QPO data

Simple item page
dc.creatorAbramowicz, M. A.
dc.creatorBarret, D.
dc.creatorBursa, M.
dc.creatorHorak, J.
dc.creatorKluzniak, W.
dc.creatorRebusco, P.
dc.creatorTorok, G.
dc.date2005-10-15
dc.date.accessioned2026-07-07T06:43:54Z
dc.date.available2026-07-07T06:43:54Z
dc.descriptionDouble peak kHz QPO frequencies in neutron star sources varies in time by a factor of hundreds Hz while in microquasar sources the frequencies are fixed and located at the line ν_2 = 1.5 ν_1 in the frequency-frequency plot. The crucial question in the theory of twin HFQPOs is whether or not those observed in neutron-star systems are essentially different from those observed in black holes. In black hole systems the twin HFQPOs are known to be in a 3:2 ratio for each source. At first sight, this seems not to be the case for neutron stars. For each individual neutron star, the upper and lower kHz QPO frequencies, ν_2 and ν_1, are linearly correlated, ν_2=A ν_1 + B, with the slope A < 1.5, i.e., the frequencies definitely are not in a 1.5 ratio. In this contribution we show that when considered jointly on a frequency-frequency plot, the data for the twin kHz QPO frequencies in several (as opposed to one) neutron stars uniquely pick out a certain preferred frequency ratio that is equal to 1.5 for the six sources examined so far.
dc.description3 pages, 1 figure, Astronomische Nachrichten, in press
dc.identifierhttps://arxiv.org/abs/astro-ph/0510462
dc.identifierhttp://arxiv.org/abs/astro-ph/0510462
dc.identifierAstron.Nachr. 326 (2005) 864-866
dc.identifierdoi:10.1002/asna.200510428
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/102594
dc.subjectAstrophysics
dc.titleThe correlations and anticorrelations in QPO data
dc.typetext

Files

Collections

arXiv