English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We present the results of our studies of the aperiodic optical fluxvariability for SS Cyg, an accreting binary systemwith a white dwarf. The mainset of observational data presented here was obtained with the ANDOR/iXonDU-888 photometer mounted on the RTT-150 telescope, which allowed a record(forCCD photometers) time resolution up to 8 ms to be achieved. The power spectraof the source's flux variability have revealed that the aperiodic variabilitycontains information about the inner boundary of the optically thick flow inthe binary system. We show that the inner boundary of the optically thickaccretion disk comes close to the white dwarf surface at the maximum of thesource's bolometric light curve, i.e., at the peak of the instantaneousaccretion rate onto the white dwarf, while the optically thick accretion diskis truncated at distances 8.5e9 cm ~10 R_{WD} in the low state. We suggest thatthe location of the inner boundary of the accretion disk in the binary can betraced by studying the parameters of the power spectra for accreting whitedwarfs. In particular, this allows the mass of the accreting object to beestimated.

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