J/A+A/553/A127ivo://CDS.VizieR/J/A+A/553/A127doi:10.26093/cds/vizier.35530127CDSPapics P.I.Tkachenko A.Aerts C.Briquet M.Marcos-Arenal P.,Beck P.G.Uytterhoeven K.Trivino Hage A.Southworth J.Clubb K.I.,Bloemen S.Degroote P.Jackiewicz J.McKeever J.Van Winckel H.,Niemczura E.Gameiro J.F.Debosscher J.2013-10-20T09:36:20Z2013-05-23T08:31:51ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frvariable-starsb-starsOB stars are important in the chemistry and evolution of the Universe, but the sample of targets that is well understood from an asteroseismological point of view is still too limited to provide feedback on the current evolutionary models. We extend this sample with two spectroscopic binary systems. Our goal is to provide orbital solutions, fundamental parameters, and abundances from disentangled high-resolution high signal-to-noise spectra, as well as to analyse and interpret the variations in the Kepler light curve of these carefully selected targets. This way we continue our efforts to map the instability strips of beta Cep and slowly pulsating B stars using the combination of high-resolution ground-based spectroscopy and uninterrupted space-based photometry. We fit Keplerian orbits to radial velocities measured from selected absorption lines of high-resolution spectroscopy using synthetic composite spectra to obtain orbital solutions. We used revised masks to obtain optimal light curves from the original pixel-data from the Kepler satellite, which provided better long-term stability compared to the pipeline-processed light curves. We used various time-series analysis tools to explore and describe the nature of variations present in the light curve. We find two eccentric double-lined spectroscopic binary systems containing a total of three main sequence B-type stars (and one F-type component), of which at least one in each system exhibits light variations. The light curve analysis (combined with spectroscopy) of the system of two B stars points towards the presence of tidally excited g modes in the primary component. We interpret the variations seen in the second system as classical g mode pulsations driven by the kappa mechanism in the B type primary, and explain the unexpected power in the p mode region as the result of nonlinear resonant mode excitation.2013A&A...553A.127Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/553/A127CatalogResearchIsServedByTAP VizieR generic servicerelated-toV/133 : Kepler Input Catalog (Kepler Mission Team, 2009)J/A+A/393/965 : Slowly pulsating B stars intrinsic frequencies (de Cat+, 2003)J/A+A/506/111 : Frequency analysis of HD 180642 (V1449 Aql) (Degroote+, 2009)J/A+A/506/471 : Frequency analysis of CoRoT B stars (Degroote+, 2009)J/A+A/525/A23 : Frequency analysis of HD 49434 (Mathias+, 2011)J/A+A/544/A106 : p-mode frequencies of the solar twin 18 Sco (Bazot+, 2012)J/A+A/549/A104 : The Kepler delta Scuti star KIC 5988140 (Lampens+, 2013)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/553/A127https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/553/A127http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/553/A127https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/553/A127https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/553/A127http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/553/A127GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/553/A127/tablea1Fourier parameters for KIC 4931738recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintf[0.004/22] Frequencyd**-1em.freqdoublee_fFrequency errord**-1stat.errordoubleAAmplitude (in 10^-6^)(10-6)src.var.amplitudefloate_AAmplitude error(10-6)stat.errorfloattheta[-0.5/0.5] Phase {theta}={phi}(rad)/{pi}time.phasefloate_thetaPhase errorstat.error;pos.posAngfloatS/N1Signal-to-noise in a 1d^-1^ wide window around fstat.snrfloatS/N3Signal-to-noise in a 3d^-1^ wide window around fstat.snrfloatS/NfSignal-to-noise computed over full periodogramstat.snrfloatJ/A+A/553/A127/tablea2Fourier parameters for KIC 6352430recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintf[0.004/22] Frequencyd**-1em.freqdoublee_fFrequency errord**-1stat.errordoubleAAmplitude (in 10^-6^)(10-6)src.var.amplitudefloate_AAmplitude error(10-6)stat.errorfloattheta[-0.5/0.5] Phase {theta}={phi}(rad)/{pi}time.phasefloate_thetaPhase errorstat.error;pos.posAngfloatS/N1Signal-to-noise in a 1d^-1^ wide window around fstat.snrfloatS/N3Signal-to-noise in a 3d^-1^ wide window around fstat.snrfloatS/NfSignal-to-noise computed over full periodogramstat.snrfloat