Hostname: page-component-586b7cd67f-2plfb Total loading time: 0 Render date: 2024-11-27T23:15:24.263Z Has data issue: false hasContentIssue false
  • English
  • Français

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: [email protected], [email protected], [email protected] 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: [email protected], [email protected], [email protected] Department of Physics, Göteborg University, S-412 96 Göteborg, Sweden. email: [email protected] 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: [email protected], [email protected], [email protected]
Eva Šrámková
Affiliation:
Institute of Physics, Faculty of Philosophy and Science, Silesian University in Opava, Bezručovo nám. 13, CZ-74601 Opava, Czech Republic. email: [email protected], [email protected], [email protected] Copernicus Astronomical Centre, Polish Academy of Sciences, PL-00 716 Warszawa, Bartycka 18, Poland
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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

References

Abramowicz, M.A. & Kluźniak, W., 2001, A&A 374L, 19A, astro-ph/010507Google Scholar
Abramowicz, M.A. & Kluźniak, W., 2004, AIP Conference Proceedings, Vol. 714, Edited by Kaaret, Philip, Frederick, K. Lamb, and Swank, Jean H., Melville, NY: AIP, 2004, p.21-28Google Scholar
Abramowicz, M.A., Kluźniak, W., McClintock, J.E. & Remillard, R. A., 2004, ApJ 609, L63 CrossRefGoogle Scholar
Aliev, A.N. & Galtsov, D.V., 1981, Gen. Relativity Gravitation, 13, 899 CrossRefGoogle Scholar
Beer, M.E. & Podsiadlowski, P. 2002, MNRAS 331, 351 Google Scholar
Blaes, O.M., Šrámková, E., Abramowicz, M.A., Kluźniak, W. & Torkelsson, U., 2006, ApJ, submittedGoogle Scholar
Bursa, M., in Proceedings of RAGtime 6/7: Workshops on black holes and neutron stars, Opava, 16–18/18–20 September 2004/2005, edited by S. Hledík and Z. Stuchlík, Silesian University in Opava, Opava, 2005b, ISBN 80-7248-242-4 Google Scholar
Greene, J., Bailyn, Ch. D. & Orosz, J.A., 2001, ApJ 554, 1290 CrossRefGoogle Scholar
Horák, J., 2005, Astronomische Nachrichten 326, 845–848 CrossRefGoogle Scholar
Kluźniak, W., & Abramowicz, M.A., 2000, Phys. Rev. Lett., submitted, astro-ph/0105057Google Scholar
Kluźniak, W., Abramowicz, M.A., 2002, astro-ph/0203314Google Scholar
McClintock, J.E. & Remillard, R.A., 2003, astro-ph/0306213Google Scholar
McClintock, J.E., Shafee, R., Narayan, R., Remillard, R.A., Davis, S.W., Li, L.X., 2006, accepted for publication in ApJ, astro-ph/0606076 Google Scholar
Nowak, M.A. & Lehr, D.E., 1998, in Theory of Black Hole Accretion Disks, ed. Abramowicz, M.A., Björnsson, G., & Pringle, J.E. (Cambridge: Cambridge University Press), 233–253 Google Scholar
Šrámková, E., 2005, Astronomische Nachrichten, 326, 835–837 CrossRefGoogle Scholar
Török, G., 2005, Astronomische Nachrichten, 326, 856 CrossRefGoogle Scholar
Török, G., Abramowicz, M.A., Kluźniak, W. & Stuchlík, Z., 2005, A&A, 436, 1 Google Scholar
Török, G. & Stuchlík, Z., 2005, A&A, 37, 775–788 Google Scholar
Török, G., Abramowicz, M. A., Kluźniak, W. & Stuchlík, Z., 2006, in print, astro-ph/0603847 Google Scholar
van der Klis, M., 2005, Astronomische Nachrichten, 326, 798–803 CrossRefGoogle Scholar