On the change of the inner boundary of an optically thick accretion disk around white dwarfs using the dwarf nova SS Cyg as an example |
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| Authors: | M G Revnivtsev R A Burenin A Yu Tkachenko I M Khamitov T Ak A Merloni M N Pavlinsky R A Sunyaev |
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| Institution: | 1.Space Research Institute,Russian Academy of Sciences,Moscow,Russia;2.Excellence Cluster Universe,Technische Universit?t München,Garching,Germany;3.TüB?TAK National Observatory,Antalya,Turkey;4.Department of Astronomy and Space Sciences,Istanbul University,Istanbul,Turkey;5.Max-Planck-Institut für Astrophysik,Garching,Germany |
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| Abstract: | We present the results of our studies of the aperiodic optical flux variability for SS Cyg, an accreting binary systemwith
a white dwarf. The main set of observational data presented here was obtained with the ANDOR/iXon DU-888 photometer mounted
on the RTT-150 telescope, which allowed a record (for CCD photometers) time resolution up to 8 ms to be achieved. The power
spectra of the source’s flux variability have revealed that the aperiodic variability contains information about the inner
boundary of the optically thick flow in the binary system. We show that the inner boundary of the optically thick accretion
disk comes close to the white dwarf surface at the maximum of the source’s bolometric light curve, i.e., at the peak of the
instantaneous accretion rate onto the white dwarf, while the optically thick accretion disk is truncated at distances 8.5
× 109 cm ∼10R
WD in the low state. We suggest that the location of the inner boundary of the accretion disk in the binary can be traced by
studying the parameters of the power spectra for accreting white dwarfs. In particular, this allows the mass of the accreting
object to be estimated. |
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