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Title:
The correlations and anticorrelations in QPO data
Authors:
Abramowicz, M. A.; Barret, D.; Bursa, M.; Horák, J.; Kluźniak, W.; Rebusco, P.; Török, G.
Affiliation:
AA( Department of Physics, Göteborg University, 412 96 Göteborg, Sweden), AB(Centre d'Etude Spatiale des Rayonnements, CNRS/UPS, 9 Avenue du Colonel Roche, 31028 Tolouse Cedex 04, France), AC(Astronomical Institute, Academy of Sciences, Boční II 1401, 141 31 Praha 4, Czech Republic), AD(Astronomical Institute, Academy of Sciences, Boční II 1401, 141 31 Praha 4, Czech Republic), AE(Zielona Góra University, Lubuska 2, 65-265 Zielona Góra, Poland), AF(Max-Planck-Institute für Astrophysik, 85741 Garching, Germany), AG(Institute of Physics, Silesian University in Opava, Bezručovo nám. 13, 746 01 Opava, Czech Republic)
Publication:
Astronomische Nachrichten, Vol.326, Issue 9, p.864-866 (AN Homepage)
Publication Date:
11/2005
Origin:
AN
Keywords:
quasi-periodic oscillations, stars: neutron
DOI:
10.1002/asna.200510428
Bibliographic Code:
2005AN....326..864A

Abstract

Double 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 = 1.5ν_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=Aν_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.
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