KFU. Card publication. Parameters of SU UMa and WZ Sge-Type Dwarf Novae in Quiescent State. I. FL Psc, TY Psc and V455 And

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PARAMETERS OF SU UMA AND WZ SGE-TYPE DWARF NOVAE IN QUIESCENT STATE. I. FL PSC, TY PSC AND V455 AND

Form of presentation

Articles in international journals and collections

Year of publication

2023

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Authors, employees of KFU

Shimanskiy Vladislav Vladimirovich, author

Bibliographic description in the original language

Dudnik A.A. Parameters of SU UMa and WZ Sge-Type Dwarf Novae in Quiescent State. I. FL Psc, TY Psc and V455 And [Text] / A. A. Dudnik, V.V.Shimansky, N. V. Borisov, A.A.Mitrofanova, M. M. Gabdeev // Astrophysical Bulletin - 2023 - V.78. - PP.25–35.

Annotation

We present the results of model analysis of the optical spectra of SU UMa and WZ Sge-type dwarf novae TY Psc, FL Psc, and V455 And .Spectroscopic observations were carried out at the SAO RAS 6-m BTA telescope in 2013. The selection criterion for the systems under study is their existence in a quiescent state with an optically thin accretion disk and dominance of white dwarf radiation. The fulfillment of the criterion was verified by observing the H I Balmer series broad absorption lines simultaneously with two-peak H I, He I, and Fe II emissions. A technique for automated fitting of model spectra of white dwarfs and observed spectra of dwarf novae based on quantitative criteria for theirmatching is proposed and implemented. The atmospheric parameters (effective temperature Teff and surface gravity log g) of accretors in TY Psc, FL Psc, and V455 And were determined applying it and used further to obtain their masses and radii. Due to the technique proposed here we obtained the estimates of the fundamental parameters of the secondaries using the theoretical “mass–radius” relationships for brown and red main-sequence dwarfs. As a result, we demonstrate the possibility in principle of determining all the main parameters of the SU UMa and WZ Sge dwarf novae based on modeling and the analysis of a small number of their spectra in the quiescent state.

Keywords

methods: numerical?methods, observational?stars, cataclysmic variables?stars, dwarf novae?white dwarfs?stars, individual: FL Psc, TY Psc, V455 And

The name of the journal

ASTROPHYSICAL BULLETIN

URL

https://link.springer.com/article/10.1134/S1990341323010054

Please use this ID to quote from or refer to the card

https://repository.kpfu.ru/eng/?p_id=290452&p_lang=2

Full metadata record

Field DC	Value	Language
dc.contributor.author	Shimanskiy Vladislav Vladimirovich	ru_RU
dc.date.accessioned	2023-01-01T00:00:00Z	ru_RU
dc.date.available	2023-01-01T00:00:00Z	ru_RU
dc.date.issued	2023	ru_RU
dc.identifier.citation	Dudnik A.A. Parameters of SU UMa and WZ Sge-Type Dwarf Novae in Quiescent State. I. FL Psc, TY Psc and V455 And [Text] / A. A. Dudnik, V.V.Shimansky, N. V. Borisov, A.A.Mitrofanova, M. M. Gabdeev // Astrophysical Bulletin - 2023 - V.78. - PP.25–35.	ru_RU
dc.identifier.uri	https://repository.kpfu.ru/eng/?p_id=290452&p_lang=2	ru_RU
dc.description.abstract	ASTROPHYSICAL BULLETIN	ru_RU
dc.description.abstract	We present the results of model analysis of the optical spectra of SU UMa and WZ Sge-type dwarf novae TY Psc, FL Psc, and V455 And .Spectroscopic observations were carried out at the SAO RAS 6-m BTA telescope in 2013. The selection criterion for the systems under study is their existence in a quiescent state with an optically thin accretion disk and dominance of white dwarf radiation. The fulfillment of the criterion was verified by observing the H I Balmer series broad absorption lines simultaneously with two-peak H I, He I, and Fe II emissions. A technique for automated fitting of model spectra of white dwarfs and observed spectra of dwarf novae based on quantitative criteria for theirmatching is proposed and implemented. The atmospheric parameters (effective temperature Teff and surface gravity log g) of accretors in TY Psc, FL Psc, and V455 And were determined applying it and used further to obtain their masses and radii. Due to the technique proposed here we obtained the estimates of the fundamental parameters of the secondaries using the theoretical “mass–radius” relationships for brown and red main-sequence dwarfs. As a result, we demonstrate the possibility in principle of determining all the main parameters of the SU UMa and WZ Sge dwarf novae based on modeling and the analysis of a small number of their spectra in the quiescent state.	ru_RU
dc.language.iso	ru	ru_RU
dc.subject	methods: numerical?methods	ru_RU
dc.subject	observational?stars	ru_RU
dc.subject	cataclysmic variables?stars	ru_RU
dc.subject	dwarf novae?white dwarfs?stars	ru_RU
dc.subject	individual: FL Psc	ru_RU
dc.subject	TY Psc	ru_RU
dc.subject	V455 And	ru_RU
dc.title	Parameters of SU UMa and WZ Sge-Type Dwarf Novae in Quiescent State. I. FL Psc, TY Psc and V455 And	ru_RU
dc.type	Articles in international journals and collections	ru_RU