KFU. Card publication. An X-ray and Optical Study of the Dwarf Nova Candidate OGLE-BLG-DN-0064

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FEDERAL UNIVERSITY

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AN X-RAY AND OPTICAL STUDY OF THE DWARF NOVA CANDIDATE OGLE-BLG-DN-0064

Form of presentation

Articles in international journals and collections

Year of publication

2024

Язык

английский

Authors, employees of KFU

Galiullin Ilkham Irekovich, author

Kolbin Aleksandr Ivanovich, author

Shimanskiy Vladislav Vladimirovich, author

Bibliographic description in the original language

Sibgatullin A.B, Dodon V.I, Galiullin I.I, Kolbin A.I, Shimansky V.V., VinokurovA.S. An X-ray and Optical Study of the Dwarf Nova Candidate OGLE-BLG-DN-0064//Astronomy Letters. - 2024. - Vol.50, Is.11. - P.676-686.

Annotation

The source OGLE-BLG-DN-0064 (hereafter OGLE64) was classified as a potential dwarf nova based on its regular outburst activity revealed by theOGLE optical survey. In this paper we investigate the X-ray and optical emissions from the source OGLE64 based on archival Chandra and Swift X-ray data and our optical observations with the 6-m BTA telescope at the Special Astrophysical Observatory of the Russian Academy of Sciences. OGLE64 shows an X-ray luminosity LX ≈ 1.6 × 1032 erg s−1 and a high X-ray-to-optical flux ratio FX/Fopt ≈ 1.5 typical for accreting white dwarfs. The X-ray spectrum of OGLE64 is better fitted by the models of a power law with a photon index Γ ≈ 1.9 and an optically thin plasma with a temperature kT ≈ 6.4 keV. The optical spectrum shows hydrogen and neutral helium emission lines in some of which a double-peaked structure is observed. An analysis of the outburst activity of OGLE64 based on data from the OGLE, ZTF, ATLAS, and ASAS-SN optical surveys has revealed superoutbursts with a characteristic supercycle Psuper ≈ 400 days. We found no significant variability in either the X-ray or optical light curves of OGLE64 that could be associated with the change in the visibility conditions for the emitting regions at different orbital phases. Our estimates of the orbital period of the system by indirect methods show that the period probably lies in the range Porb ∼ 1.5−3.5 h. The properties of the X-ray and optical emissions from OGLE64 lead us to conclude that the system is an SU UMa-type dwarf nova.

Keywords

cataclysmic variables, dwarf novae, superoutbursts, accretion, X-ray astronomy

The name of the journal

Astronomy Letters

URL

https://www.scopus.com/inward/record.uri?eid=2-s2.0-105000928323&doi=10.1134%2fS1063773725700033&partnerID=40&md5=bc56f0a8a4aeea7017c04d77ceac05f4

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

https://repository.kpfu.ru/eng/?p_id=313340&p_lang=2

Full metadata record

Field DC	Value	Language
dc.contributor.author	Galiullin Ilkham Irekovich	ru_RU
dc.contributor.author	Kolbin Aleksandr Ivanovich	ru_RU
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	Sibgatullin A.B, Dodon V.I, Galiullin I.I, Kolbin A.I, Shimansky V.V., VinokurovA.S. An X-ray and Optical Study of the Dwarf Nova Candidate OGLE-BLG-DN-0064//Astronomy Letters. - 2024. - Vol.50, Is.11. - P.676-686.	ru_RU
dc.identifier.uri	https://repository.kpfu.ru/eng/?p_id=313340&p_lang=2	ru_RU
dc.description.abstract	Astronomy Letters	ru_RU
dc.description.abstract	The source OGLE-BLG-DN-0064 (hereafter OGLE64) was classified as a potential dwarf nova based on its regular outburst activity revealed by theOGLE optical survey. In this paper we investigate the X-ray and optical emissions from the source OGLE64 based on archival Chandra and Swift X-ray data and our optical observations with the 6-m BTA telescope at the Special Astrophysical Observatory of the Russian Academy of Sciences. OGLE64 shows an X-ray luminosity LX ≈ 1.6 × 1032 erg s−1 and a high X-ray-to-optical flux ratio FX/Fopt ≈ 1.5 typical for accreting white dwarfs. The X-ray spectrum of OGLE64 is better fitted by the models of a power law with a photon index Γ ≈ 1.9 and an optically thin plasma with a temperature kT ≈ 6.4 keV. The optical spectrum shows hydrogen and neutral helium emission lines in some of which a double-peaked structure is observed. An analysis of the outburst activity of OGLE64 based on data from the OGLE, ZTF, ATLAS, and ASAS-SN optical surveys has revealed superoutbursts with a characteristic supercycle Psuper ≈ 400 days. We found no significant variability in either the X-ray or optical light curves of OGLE64 that could be associated with the change in the visibility conditions for the emitting regions at different orbital phases. Our estimates of the orbital period of the system by indirect methods show that the period probably lies in the range Porb ∼ 1.5−3.5 h. The properties of the X-ray and optical emissions from OGLE64 lead us to conclude that the system is an SU UMa-type dwarf nova.	ru_RU
dc.language.iso	ru	ru_RU
dc.subject	cataclysmic variables	ru_RU
dc.subject	dwarf novae	ru_RU
dc.subject	superoutbursts	ru_RU
dc.subject	accretion	ru_RU
dc.subject	X-ray astronomy	ru_RU
dc.title	An X-ray and Optical Study of the Dwarf Nova Candidate OGLE-BLG-DN-0064	ru_RU
dc.type	Articles in international journals and collections	ru_RU