Volume 519, September 2010
|Number of page(s)||9|
|Section||Stellar structure and evolution|
|Published online||14 September 2010|
Wavelet and R/S analysis of the X-ray flickering of cataclysmic variables*
ICFO - Institut de Ciències Fotòniques, avinguda del Canal Olimpic s/n,
08860 Castelldefels (Barcelona), Spain e-mail: firstname.lastname@example.org
2 Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 3, 35122 Padova, Italy e-mail: [fabrizio.tamburini;antonio.bianchini]@unipd.it
3 INAF - Osservatorio Astronomico di Capodimonte, salita Moiariello 16, 80131 Napoli, Italy e-mail: email@example.com
Accepted: 31 May 2010
Context. Recently, wavelets and R/S analysis have been used as statistical tools to characterize the optical flickering of cataclysmic variables.
Aims. Here we present the first comprehensive study of the statistical properties of X-ray flickering of cataclysmic variables in order to link them with physical parameters.
Methods. We analyzed a sample of 97 X-ray light curves of 75 objects of all classes observed with the XMM-Newton space telescope. By using the wavelets analysis, each light curve has been characterized by two parameters, α and Σ, that describe the energy distribution of flickering on different timescales and the strength at a given timescale, respectively. We also used the R/S analysis to determine the Hurst exponent of each light curve and define their degree of stochastic memory in time.
Results. The X-ray flickering is typically composed of long time scale events (1.5 α 3), with very similar strengths in all the subtypes of cataclysmic variables (-3 Σ -1.5). The X-ray data are distributed in a much smaller area of the α - Σ parameter space with respect to those obtained with optical light curves. The tendency of the optical flickering in magnetic systems to show higher Σ values than the non-magnetic systems is not encountered in the X-rays. The Hurst exponents estimated for all light curves of the sample are larger than those found in the visible, with a peak at 0.82. In particular, we do not obtain values lower than 0.5. The X-ray flickering presents a persistent memory in time, which seems to be stronger in objects containing magnetic white dwarf primaries.
Conclusions. The similarity of the X-ray flickering in objects of different classes together with the predominance of a persistent stochastic behavior can be explained in terms of magnetically-driven accretion processes acting in a considerable fraction of the analyzed objects.
Key words: novae, cataclysmic variables / X-rays: binaries / accretion, accretion disks / magnetic fields / methods: data analysis
Table 1 is only available in electronic form at http://www.aanda.org
© ESO, 2010
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