Volume 545, September 2012
|Number of page(s)||8|
|Section||Stellar structure and evolution|
|Published online||05 September 2012|
A possible interpretation for the apparent differences in LFQPO types in microquasars
APC, AstroParticule & Cosmologie, UMR 7164 CNRS/N2P3,
Université Paris Diderot, CEA/Irfu, Observatoire de Paris,
Sorbonne Paris Cité, 10 rue Alice Domon et Léonie
Paris Cedex 13,
2 Laboratoire de Physique et Chimie de l’Environnement et de l’Espace, Université d’Orléans/CNRS, Orléans, France
3 Laboratoire AIM, CEA/IRFU-CNRS/INSU-Université Paris Diderot, CEA DSM/IRFU/SAp, Centre de Saclay, 91191 Gif-sur-Yvette, France
Accepted: 23 July 2012
Aims. In most microquasars, low-frequency quasi-periodic oscillations (LFQPO) have been classified into three types (A, B and C depending on the peak distribution in the power density spectra and the shape of the noise) but no explanationhas been proposed yet. The accretion-ejection instability (AEI) was presented in 1999 as a possible explanation for the fast varying LFQPO that occur most often. Here we look at a possible generalization to explain the characteristics of the other two LFQPO types.
Methods. It was recently shown that when the disk approaches its last stable orbit, the AEI is markedly affected by relativistic effects. We focus on the characteristics of the LFQPO that would result from the relativistic AEI and compare them with the different LFQPO types.
Results. The effects of relativity on the AEI seem to be able to explain most of the characteristics of the three types of LFQPO within one formalism.
Key words: X-rays: binaries / instabilities / accretion, accretion disks
© ESO, 2012
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