Quasi-periodic oscillations in accreting magnetic white dwarfs: I. Observational constraints in X-ray and optical

Quasi-periodic oscillations (QPOs) are observed in the optical flux of some polars with typical periods of 1 to 3 s but none have been observed yet in X-rays where a significant part of the accreting energy is released. QPOs are expected and predicted from shock oscillations. Most of the polars have...

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Bibliographic Details
Published in:Astronomy and astrophysics (Berlin) 2015-07, Vol.579, p.A24
Main Authors: Bonnet-Bidaud, J M, Mouchet, M, Busschaert, C, Falize, E, Michaut, C
Format: Article
Language:English
Subjects:
Accretion
Astronomy
Astrophysics
Flux
Oscillations
Physics
Quasi-Periodic Oscillations
White dwarf stars
X-rays
XMM (spacecraft)
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Summary:Quasi-periodic oscillations (QPOs) are observed in the optical flux of some polars with typical periods of 1 to 3 s but none have been observed yet in X-rays where a significant part of the accreting energy is released. QPOs are expected and predicted from shock oscillations. Most of the polars have been observed by the XMM-Newton satellite. We made use of the homogeneous set of observations of the polars by XMM-Newton to search for the presence of QPOs in the (0.5-10 keV) energy range and to set significant upper limits for the brightest X-ray polars. We extracted high time-resolution X-ray light curves by taking advantage of the 0.07 s resolution of the EPICPN camera. The absence of X-ray QPOs imposes an upper limit of ~(5-10) g cm[sup 2] s[sup -1] on the specific accretion rate but this condition is found inconsistent with the value required to account for the amplitudes and frequencies of the observed optical QPOs. This contradiction outlines probable shortcomings with the shock instability model.
ISSN:0004-6361
1432-0746
1432-0756
DOI:10.1051/0004-6361/201425482