KFU. Card publication. Parameters of SU UMa and WZ Sge-Type Dwarf Novae in Quiescent State. II. V355 UMa, V521 Peg, VY Aqr, PQ And

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PARAMETERS OF SU UMA AND WZ SGE-TYPE DWARF NOVAE IN QUIESCENT STATE. II. V355 UMA, V521 PEG, VY AQR, PQ AND

Form of presentation

Articles in Russian journals and collections

Year of publication

2024

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Authors, employees of KFU

Shimanskiy Vladislav Vladimirovich, author

Bibliographic description in the original language

Shimansky V.V. Parameters of SU UMa and WZ Sge-Type Dwarf Novae in Quiescent State. II. V355 UMa, V521 Peg, VY Aqr, PQ And [Text] / V. V. Shimansky, A.A. Dudnik, N. V. Borisov, S.S. Kotov // Astrophysical Bulletin - 2024 - V.79. - PP.359–367.

Annotation

Using a previously developed technique, a study of moderate-resolution optical spectra was carried out, and sets of parameters for the dwarf novae V355UMa, V521Peg, VYAqr, and PQAnd were obtained. Observations of the systems in late relaxation phases after a burst or in a quiescent state were carried out in 2020 and 2021 with the 6-m BTA telescope of SAO RAS. Their analysis took into account the requirement for an optimum description of the observed absorption profiles of the Balmer series lines with the model spectra of white dwarfs with radiative and convective transfer. As a result, the atmospheric parameters of the primaries were determined for all the systems, and when they were subsequently compared with models of the internal structure of white-dwarf and main-sequence stars, sets of fundamental parameters of the objects were also determined. It has been established that analysis of the spectra of dwarf novae containing moderately cool white dwarfs with Teff = 12 000–15 000 K provides better accuracy of their parameters than systems with hotter primaries. A simultaneous condition to be fulfilled for increasing accuracy is to carry out observations after the objects relax to a quiescent state, since the emission lines of the accretion disk significantly narrow the region of the analyzed spectrum. It has been found that the primary components of V355UMa, V521 Peg, VYAqr, and PQAnd have masses within the range ofM1 = 0.59–0.87M⊙, and their cool companions are red dwarfs withM2 = 0.11–0.13M⊙.

Keywords

observations: spectroscopy?stars: white dwarfs, dwarf novae?methods: atmosphere models?individual: V355UMa, V521 Peg, VYAqr, PQAnd

The name of the journal

ASTROPHYSICAL BULLETIN

URL

https://www.sao.ru/Doc-k8/Science/Public/Bulletin/Vol79/N3/ASPB-79-03-443Sh.html

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

https://repository.kpfu.ru/eng/?p_id=302624&p_lang=2

Full metadata record

Field DC	Value	Language
dc.contributor.author	Shimanskiy Vladislav Vladimirovich	ru_RU
dc.date.accessioned	2024-01-01T00:00:00Z	ru_RU
dc.date.available	2024-01-01T00:00:00Z	ru_RU
dc.date.issued	2024	ru_RU
dc.identifier.citation	Shimansky V.V. Parameters of SU UMa and WZ Sge-Type Dwarf Novae in Quiescent State. II. V355 UMa, V521 Peg, VY Aqr, PQ And [Text] / V. V. Shimansky, A.A. Dudnik, N. V. Borisov, S.S. Kotov // Astrophysical Bulletin - 2024 - V.79. - PP.359–367.	ru_RU
dc.identifier.uri	https://repository.kpfu.ru/eng/?p_id=302624&p_lang=2	ru_RU
dc.description.abstract	ASTROPHYSICAL BULLETIN	ru_RU
dc.description.abstract	Using a previously developed technique, a study of moderate-resolution optical spectra was carried out, and sets of parameters for the dwarf novae V355UMa, V521Peg, VYAqr, and PQAnd were obtained. Observations of the systems in late relaxation phases after a burst or in a quiescent state were carried out in 2020 and 2021 with the 6-m BTA telescope of SAO RAS. Their analysis took into account the requirement for an optimum description of the observed absorption profiles of the Balmer series lines with the model spectra of white dwarfs with radiative and convective transfer. As a result, the atmospheric parameters of the primaries were determined for all the systems, and when they were subsequently compared with models of the internal structure of white-dwarf and main-sequence stars, sets of fundamental parameters of the objects were also determined. It has been established that analysis of the spectra of dwarf novae containing moderately cool white dwarfs with Teff = 12 000–15 000 K provides better accuracy of their parameters than systems with hotter primaries. A simultaneous condition to be fulfilled for increasing accuracy is to carry out observations after the objects relax to a quiescent state, since the emission lines of the accretion disk significantly narrow the region of the analyzed spectrum. It has been found that the primary components of V355UMa, V521 Peg, VYAqr, and PQAnd have masses within the range ofM1 = 0.59–0.87M⊙, and their cool companions are red dwarfs withM2 = 0.11–0.13M⊙.	ru_RU
dc.language.iso	ru	ru_RU
dc.subject	observations: spectroscopy?stars: white dwarfs	ru_RU
dc.subject	dwarf novae?methods: atmosphere models?individual: V355UMa	ru_RU
dc.subject	V521 Peg	ru_RU
dc.subject	VYAqr	ru_RU
dc.subject	PQAnd	ru_RU
dc.title	Parameters of SU UMa and WZ Sge-Type Dwarf Novae in Quiescent State. II. V355 UMa, V521 Peg, VY Aqr, PQ And	ru_RU
dc.type	Articles in Russian journals and collections	ru_RU