Mode identification in the high-amplitude ? Scuti star V2367 Cyg

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dc.authoridUlusoy, Ceren/0000-0001-8868-5558
dc.authoridFox-Machado, Lester/0000-0002-2781-873X
dc.authoridIliev, Ilian/0000-0002-9811-449X
dc.authoridCARBOGNANI, Albino/0000-0002-0737-7068
dc.authoridBalona, Luis/0000-0003-1241-9792
dc.authoridDimitrov, Dinko/0000-0002-1667-5868
dc.authorwosidDimitrov, Dinko P./J-7682-2013
dc.authorwosidUlusoy, Ceren/N-6339-2013
dc.authorwosidMoody, Michael P/H-9377-2013
dc.authorwosidFox-Machado, Lester/L-5746-2019
dc.authorwosidIliev, Ilian/W-7098-2018
dc.contributor.authorUlusoy, C.
dc.contributor.authorGuelmez, T.
dc.contributor.authorStateva, I.
dc.contributor.authorDimitrov, D.
dc.contributor.authorIliev, I. Kh
dc.contributor.authorKobulnicky, H. A.
dc.contributor.authorYasarsoy, B.
dc.date.accessioned2024-08-04T20:37:25Z
dc.date.available2024-08-04T20:37:25Z
dc.date.issued2013
dc.departmentİnönü Üniversitesien_US
dc.description.abstractWe report on a multisite photometric campaign on the high-amplitude delta Scuti star V2367 Cyg in order to determine the pulsation modes. We also used high-dispersion spectroscopy to estimate the stellar parameters and projected rotational velocity. Time series multicolour photometry was obtained during a 98-d interval from five different sites. These data were used together with model atmospheres and non-adiabatic pulsation models to identify the spherical harmonic degree of the three independent frequencies of highest amplitude as well as the first two harmonics of the dominant mode. This was accomplished by matching the observed relative light amplitudes and phases in different wavebands with those computed by the models. In general, our results support the assumed mode identifications in a previous analysis of Kepler data.en_US
dc.description.sponsorshipSouth African National Research Foundation [73446]; NRF; Bulgarian NSF [DO 02-85, DO 02-362, DDVU 02/40-2010]; South African Astronomical Observatory; UNAM [PAPIIT IN104612]; CONACyT [CC-118611]; European Union; Autonomous Region of the Aosta Valley; Italian Department for Work, Health and Pensions; Regional Government of the Aosta Valley; Town Municipality of Nus; Mont Emilius Community; National Research Foundation of South Africa; Grants-in-Aid for Scientific Research [22000005] Funding Source: KAKENen_US
dc.description.sponsorshipCU sincerely thanks the South African National Research Foundation for the prize of innovation post doctoral fellowship with the grant number 73446. TG would like to thank NRF Equipment-Related Mobility Grant-2011 for travel to Turkey to carry out the photometric observations. IS and II gratefully acknowledge the partial support from Bulgarian NSF under grant DO 02-85. DD acknowledges for the support of grants DO 02-362 and DDVU 02/40-2010 of Bulgarian NSF. LAB thanks the South African National Research Foundation and the South African Astronomical Observatory for generous financial support. HAK acknowledges Carlos Vargas-Alvarez, Michael J. Lundquist, Garrett Long, Jessie C. Runnoe, Earl S. Wood, Michael J. Alexander for helping with the observations at WIRO. BY wishes to thank EUO for the allocation time of observations during the campaign. LFM acknowledges financial support from the UNAM under grant PAPIIT IN104612 and from CONACyT by way of grant CC-118611. MD, AC and DC are supported by grants provided by the European Union, the Autonomous Region of the Aosta Valley and the Italian Department for Work, Health and Pensions. The OAVdA is supported by the Regional Government of the Aosta Valley, the Town Municipality of Nus and the Mont Emilius Community. TEP acknowledges support from the National Research Foundation of South Africa. This study made use of IRAF Data Reduction and Analysis System and the Vienna Atomic Line Data Base (VALD) services. The authors thank Dr Zima for providing the FAMIAS code.en_US
dc.identifier.doi10.1093/mnras/sts293
dc.identifier.endpage3558en_US
dc.identifier.issn0035-8711
dc.identifier.issue4en_US
dc.identifier.scopus2-s2.0-84873727305en_US
dc.identifier.scopusqualityN/Aen_US
dc.identifier.startpage3551en_US
dc.identifier.urihttps://doi.org/10.1093/mnras/sts293
dc.identifier.urihttps://hdl.handle.net/11616/95951
dc.identifier.volume428en_US
dc.identifier.wosWOS:000318232000057en_US
dc.identifier.wosqualityQ1en_US
dc.indekslendigikaynakWeb of Scienceen_US
dc.indekslendigikaynakScopusen_US
dc.language.isoenen_US
dc.publisherOxford Univ Pressen_US
dc.relation.ispartofMonthly Notices of The Royal Astronomical Societyen_US
dc.relation.publicationcategoryMakale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanıen_US
dc.rightsinfo:eu-repo/semantics/openAccessen_US
dc.subjectstars: individual: V2367 Cygen_US
dc.subjectstars: oscillationsen_US
dc.subjectstars: variables: delta Scutien_US
dc.titleMode identification in the high-amplitude ? Scuti star V2367 Cygen_US
dc.typeArticleen_US

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