Please use this identifier to cite or link to this item: http://elar.urfu.ru/handle/10995/101979
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dc.contributor.authorKozhevnikov, V. P.en
dc.date.accessioned2021-08-31T15:01:01Z-
dc.date.available2021-08-31T15:01:01Z-
dc.date.issued2018-
dc.identifier.citationKozhevnikov V. P. Discovery of deep eclipses in the cataclysmic variable IPHAS J051814.33+294113.0 / V. P. Kozhevnikov. — DOI 10.1007/s10509-018-3351-9 // Astrophysics and Space Science. — 2018. — Vol. 363. — Iss. 6. — 130.en
dc.identifier.issn0004640X-
dc.identifier.otherFinal2
dc.identifier.otherAll Open Access, Green3
dc.identifier.otherhttps://www.scopus.com/inward/record.uri?eid=2-s2.0-85047620305&doi=10.1007%2fs10509-018-3351-9&partnerID=40&md5=12c650de768e5ce7ae53be9c82b7a128
dc.identifier.otherhttp://arxiv.org/pdf/1805.07065m
dc.identifier.urihttp://elar.urfu.ru/handle/10995/101979-
dc.description.abstractPerforming the photometric observations of the cataclysmic variable IPHAS J051814.33+294113.0, we discovered very deep eclipses. The observations were obtained over 14 nights, had a total duration of 56 hours and covered one year. The large time span, during which we observed the eclipses, allowed us to measure the orbital period in IPHAS J051814.33+294113.0 with high precision, Porb= 0.20603098 ± 0.00000025 d. The prominent parts of the eclipses lasted 0.1 ± 0.01 phases or 30±3min. The depth of the eclipses was variable in the range 1.8–2.9 mag. The average eclipse depth was equal to 2.42±0.06mag. The prominent parts of the eclipses revealed a smooth and symmetric shape. We derived the eclipse ephemeris, which, according to the precision of the orbital period, has a formal validity time of 500 years. This ephemeris can be useful for future investigations of the long-term period changes. During the latter four observational nights in 2017 January, we observed the sharp brightness decrease of IPHAS J051814.33+294113.0 by 2.3 mag. This brightness decrease imitated the end of the dwarf nova outburst. However, the long-term light curve of IPHAS J051814.33+294113.0 obtained in the course of the Catalina Sky Survey during 8 years showed no dwarf nova outbursts. From this we conclude that IPHAS J051814.33+294113.0 is a novalike variable. Moreover, the sharp brightness decrease, which we observed in IPHAS J051814.33+294113.0, suggests that this novalike variable belongs to the VY Scl-subtype. Due to very deep eclipses, IPHAS J051814.33+294113.0 is suitable to study the accretion disc structure using eclipse mapping techniques. Because this novalike variable has the long orbital period, it is of interest to determine the masses of the stellar components from radial velocity measurements. Then, our precise eclipse ephemeris can be useful to the phasing of spectroscopic data. © 2018, Springer Science+Business Media B.V., part of Springer Nature.en
dc.format.mimetypeapplication/pdfen
dc.language.isoenen
dc.publisherSpringer Netherlandsen
dc.rightsinfo:eu-repo/semantics/openAccessen
dc.sourceAstrophys. Space Sci.2
dc.sourceAstrophysics and Space Scienceen
dc.subjectBINARIES: ECLIPSINGen
dc.subjectNOVAE, CATACLYSMIC VARIABLESen
dc.subjectSTARS: INDIVIDUAL, IPHAS J051814.33+294113.0en
dc.titleDiscovery of deep eclipses in the cataclysmic variable IPHAS J051814.33+294113.0en
dc.typeArticleen
dc.typeinfo:eu-repo/semantics/articleen
dc.typeinfo:eu-repo/semantics/publishedVersionen
dc.identifier.rsi35500268-
dc.identifier.doi10.1007/s10509-018-3351-9-
dc.identifier.scopus85047620305-
local.contributor.employeeKozhevnikov, V.P., Astronomical Observatory, Ural Federal University, Lenin Av. 51, Ekaterinburg, 620083, Russian Federation
local.issue6-
local.volume363-
local.contributor.departmentAstronomical Observatory, Ural Federal University, Lenin Av. 51, Ekaterinburg, 620083, Russian Federation
local.identifier.pure7276877-
local.identifier.pureeb198b86-9791-4944-8232-91eda3e98812uuid
local.description.order130-
local.identifier.eid2-s2.0-85047620305-
Appears in Collections:Научные публикации ученых УрФУ, проиндексированные в SCOPUS и WoS CC

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