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dc.contributor.authorMERLONI, A.
dc.contributor.authorSunyaev, R. A.
dc.contributor.authorAk, Tansel
dc.contributor.authorKHAMITOV, I. M.
dc.contributor.authorPAVLINSKY, M. N.
dc.contributor.authorREVNIVTSEV, M. G.
dc.contributor.authorBURENIN, R. A.
dc.contributor.authorTKACHENKO, A. Yu
dc.date.accessioned2021-03-05T07:45:02Z
dc.date.available2021-03-05T07:45:02Z
dc.date.issued2012
dc.identifier.citationREVNIVTSEV M. G. , BURENIN R. A. , TKACHENKO A. Y. , KHAMITOV I. M. , Ak T., MERLONI A., PAVLINSKY M. N. , Sunyaev R. A. , "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", ASTRONOMY LETTERS-A JOURNAL OF ASTRONOMY AND SPACE ASTROPHYSICS, cilt.38, ss.238-248, 2012
dc.identifier.issn1063-7737
dc.identifier.otherav_9571f562-fa07-440b-8cc3-20b400ad59a3
dc.identifier.othervv_1032021
dc.identifier.urihttp://hdl.handle.net/20.500.12627/100613
dc.identifier.urihttps://doi.org/10.1134/s1063773712040044
dc.description.abstractWe 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 x 10(9) cm similar to 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.
dc.language.isoeng
dc.subjectFizik
dc.subjectAstronomi ve Astrofizik
dc.subjectTemel Bilimler
dc.subjectASTRONOMİ VE ASTROFİZİK
dc.subjectUzay bilimi
dc.subjectTemel Bilimler (SCI)
dc.titleOn the change of the inner boundary of an optically thick accretion disk around white dwarfs using the dwarf nova SS Cyg as an example
dc.typeMakale
dc.relation.journalASTRONOMY LETTERS-A JOURNAL OF ASTRONOMY AND SPACE ASTROPHYSICS
dc.contributor.departmentRussian Academy of Sciences , ,
dc.identifier.volume38
dc.identifier.issue4
dc.identifier.startpage238
dc.identifier.endpage248
dc.contributor.firstauthorID53806


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