Please use this identifier to cite or link to this item: https://hdl.handle.net/11147/10663
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dc.contributor.authorUlusoy, Ceren-
dc.contributor.authorUlas, B.-
dc.contributor.authorGuelmez, T.-
dc.contributor.authorBalona, L. A.-
dc.contributor.authorStateva, I.-
dc.contributor.authorIliev, I. Kh.-
dc.contributor.authorCarbognani, A.-
dc.date.accessioned2021-01-24T18:47:25Z-
dc.date.available2021-01-24T18:47:25Z-
dc.date.issued2013-
dc.identifier.issn1365-2966-
dc.identifier.issn0035-8711-
dc.identifier.urihttps://doi.org/10.1093/mnras/stt731-
dc.identifier.urihttps://hdl.handle.net/10663-
dc.description.abstractWe present results of a multisite photometric campaign on the high-amplitude delta Scuti star KIC 6382916 in the Kepler field. The star was observed over a 85-d interval at five different sites in North America and Europe during 2011. Kepler photometry and ground-based multicolour light curves of KIC 6382916 are used to investigate the pulsational content and to identify the principal modes. High-dispersion spectroscopy was also obtained in order to derive the stellar parameters and projected rotational velocity. From an analysis of the Kepler time series, three independent frequencies and a few hundred combination frequencies are found. The light curve is dominated by two modes with frequencies f(1) = 4.9107 and f(2) = 6.4314 d(-1). The third mode with f(3) = 8.0350 d(-1) has a much lower amplitude. We attempt mode identification by examining the amplitude ratios and phase differences in different wavebands from multicolour photometry and comparing them to calculations for different spherical harmonic degree, l. We find that the theoretical models for f(1) and f(2) are in a best agreement with the observations and lead to value of l = 1 modes, but the mode identification of f(3) is uncertain due to its low amplitude. Non-adiabatic pulsation models show that frequencies below 6 d(-1) are stable, which means that the low frequency of f(1) cannot be reproduced. This is a further confirmation that current models predict a narrower pulsation frequency range than actually observed.en_US
dc.description.sponsorshipNASANational Aeronautics & Space Administration (NASA); South African National Research Foundation (NRF)National Research Foundation - South Africa [73446]; South African National Research FoundationNational Research Foundation - South Africa; South African Astronomical ObservatoryNational Research Foundation - South Africa; Bulgarian NSFNational Science Fund of Bulgaria [DO 02-85, DO 02-362, DDVU 02/40-2010]; UNAMUniversidad Nacional Autonoma de Mexico [PAPIIT 104612]; CONACYTConsejo Nacional de Ciencia y Tecnologia (CONACyT) [118611]; European UnionEuropean Union (EU); Autonomous Region of the Aosta ValleyRegione Valle d'Aosta; 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 AfricaNational Research Foundation - South Africa; [HDYF-051]en_US
dc.description.sponsorshipThe authors acknowledge the whole Kepler team for providing the unprecedented data sets that make these results possible. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. CU sincerely thanks the South African National Research Foundation (NRF) for the award of innovation post-doctoral fellowship, grant no. 73446. BU is supported by the project numbered HDYF-051. TG would like to thank NRF Equipment-Related Mobility Grant-2011 for travelling to carry out the photometric observations. LAB thanks the South African National Research Foundation and the South African Astronomical Observatory for generous financial support. 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. HAK acknowledges Carlos Vargas-Alvarez, Michael J. Lundquist, Garrett Long, Jessie C. Runnoe, Earl S. Wood and Michael J. Alexander for helping with the observations at WIRO. LFM acknowledges financial support from the UNAM under grant PAPIIT 104612 and from CONACYT by the way of grant 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.language.isoenen_US
dc.publisherOxford University Pressen_US
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen_US
dc.rightsinfo:eu-repo/semantics/openAccessen_US
dc.subjectstars: individual: KIC 6382916en_US
dc.subjectstars: oscillationsen_US
dc.subjectstars: variables: delta Scutien_US
dc.titleMultisite photometric campaign on the high-amplitude delta Scuti star KIC 6382916en_US
dc.typeArticleen_US
dc.institutionauthorUlusoy, Ceren-
dc.departmentİzmir Institute of Technology. Physicsen_US
dc.identifier.volume433en_US
dc.identifier.issue1en_US
dc.identifier.startpage394en_US
dc.identifier.endpage401en_US
dc.identifier.wosWOS:000321461200032en_US
dc.relation.publicationcategoryMakale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanıen_US
dc.identifier.doi10.1093/mnras/stt731-
dc.relation.doi10.1093/mnras/stt731en_US
dc.coverage.doi10.1093/mnras/stt731en_US
dc.identifier.wosqualityQ1-
dc.identifier.scopusqualityQ1-
item.openairetypeArticle-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
item.grantfulltextnone-
item.fulltextNo Fulltext-
item.languageiso639-1en-
item.cerifentitytypePublications-
Appears in Collections:WoS İndeksli Yayınlar Koleksiyonu / WoS Indexed Publications Collection
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