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QPOs in Microquasars: the Spin Problem

Published online by Cambridge University Press:  09 August 2007

Gabriel Török ,
Marek A. Abramowicz ,
Zdeněk Stuchlík  and
Eva Šrámková
Gabriel Török
Affiliation:
Institute of Physics, Faculty of Philosophy and Science, Silesian University in Opava, Bezručovo nám. 13, CZ-74601 Opava, Czech Republic. email: terek@volny.cz, zdenek.stuchlik@fpf.slu.cz, sram_eva@centrum.cz Copernicus Astronomical Centre, Polish Academy of Sciences, PL-00 716 Warszawa, Bartycka 18, Poland
Marek A. Abramowicz
Affiliation:
Institute of Physics, Faculty of Philosophy and Science, Silesian University in Opava, Bezručovo nám. 13, CZ-74601 Opava, Czech Republic. email: terek@volny.cz, zdenek.stuchlik@fpf.slu.cz, sram_eva@centrum.cz Department of Physics, Göteborg University, S-412 96 Göteborg, Sweden. email: marek@fy.chalmers.se Copernicus Astronomical Centre, Polish Academy of Sciences, PL-00 716 Warszawa, Bartycka 18, Poland
Zdeněk Stuchlík
Affiliation:
Institute of Physics, Faculty of Philosophy and Science, Silesian University in Opava, Bezručovo nám. 13, CZ-74601 Opava, Czech Republic. email: terek@volny.cz, zdenek.stuchlik@fpf.slu.cz, sram_eva@centrum.cz
Eva Šrámková
Affiliation:
Institute of Physics, Faculty of Philosophy and Science, Silesian University in Opava, Bezručovo nám. 13, CZ-74601 Opava, Czech Republic. email: terek@volny.cz, zdenek.stuchlik@fpf.slu.cz, sram_eva@centrum.cz Copernicus Astronomical Centre, Polish Academy of Sciences, PL-00 716 Warszawa, Bartycka 18, Poland
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Abstract

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In Galactic microquasars with double-peak kHz quasi-periodic oscillations (QPOs), the ratio of the two frequencies is 3:2. This supports the suggestion that double-peak kHz QPOs are due to a non-linear resonance between two modes of accretion disk oscillations. For the microquasars with known mass, we briefly compare the black hole spin estimates based on the orbital resonance model with the recently reported spin predictions obtained by fitting the spectral continua. Results of these two approaches are not in good agreement. We stress that if the spectral fit estimates are accurate and can be taken as referential (which is still questionable), the disagreement between the predicted and referential values would represent a rather generic problem for any relativistic QPO model, as no spin influence would appear in the observed 1/M scaling of the QPO frequencies. The epicyclic frequencies relevant in these models are often considered to be equal to those of a test particle motion. However modifications of the frequencies due to disc pressure or other non-geodesic effects may play an important role, and the inaccuracy introduced in the spin estimates by the test particle approximation could be crucial.

Keywords

Black hole physicsX-rays: binaries
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S240: Binary Stars as Critical Tools & Tests in Contemporary Astrophysics , August 2006 , pp. 724 - 726
Copyright
Copyright © International Astronomical Union 2007

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