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Periodic mass-loss episodes due to an oscillation mode with variable amplitude in the hot supergiant HD 50064

dc.contributor.authorAerts, C.
dc.contributor.authorLefever, K.
dc.contributor.authorBaglin, A.
dc.contributor.authorDegroote, P.
dc.contributor.authorOreiro, R.
dc.contributor.authorVučković, M.
dc.contributor.authorSmolders, K.
dc.contributor.authorAcke, B.
dc.contributor.authorVerhoelst, T.
dc.contributor.authorDesmet, M.
dc.contributor.authorGodart, M.
dc.contributor.authorNoels, A.
dc.contributor.authorDupret, M.-A.
dc.contributor.authorAuvergne, M.
dc.contributor.authorBaudin, F.
dc.contributor.authorCatala, C.
dc.contributor.authorMichel, E.
dc.contributor.authorSamadi, R.
dc.date2010
dc.date.accessioned2016-04-05T10:30:19Z
dc.date.available2016-04-05T10:30:19Z
dc.identifier.urihttps://orfeo.belnet.be/handle/internal/3253
dc.descriptionAims. We aim to interpret the photometric and spectroscopic variability of the luminous blue variable supergiant HD 50064 (V = 8.21). Methods. CoRoT space photometry and follow-up high-resolution spectroscopy with a time base of 137 d and 169 d, respectively, was gathered, analysed, and interpreted using standard time series analysis and light curve modelling methods, as well as spectral line diagnostics. Results. The space photometry reveals one period of 37 d, which undergoes a sudden amplitude change with a factor 1.6. The pulsation period is confirmed in the spectroscopy, which additionally reveals metal line radial velocity values differing by ∼30 km s-1 depending on the spectral line and on the epoch. We estimate Teff ∼13 500 K, log g ∼ 1.5 from the equivalent width of Si lines. The Balmer lines reveal that the star undergoes episodes of changing mass loss on a time scale similar to the changes in the photometric and spectroscopic variability, with an average value of log ̇M -5 (in M⊙. yr-1). We tentatively interpret the 37 d period as the result of a strange mode oscillation.
dc.titlePeriodic mass-loss episodes due to an oscillation mode with variable amplitude in the hot supergiant HD 50064
dc.typeArticle
dc.subject.frascatiPhysical sciences
dc.audienceScientific
dc.subject.freeAsteroseismology
dc.subject.freeAverage values
dc.subject.freeBalmer lines
dc.subject.freeEquivalent width
dc.subject.freeHigh-resolution spectroscopy
dc.subject.freeLight curves
dc.subject.freeLuminous Blue Variables
dc.subject.freeMass loss
dc.subject.freeMetal line
dc.subject.freeModelling method
dc.subject.freeOscillation mode
dc.subject.freeOutflows-stars
dc.subject.freeRadial velocity
dc.subject.freeSpectral line
dc.subject.freeStars: individual
dc.subject.freeStars: oscillation
dc.subject.freeTime-scales
dc.subject.freeVariable amplitudes
dc.subject.freePhotometers
dc.subject.freePhotometry
dc.subject.freeSpectroscopic analysis
dc.subject.freeSpectroscopy
dc.subject.freeTime series
dc.subject.freeTime series analysis
dc.subject.freeStars
dc.source.titleAstronomy and Astrophysics
dc.source.volume513
dc.source.pageL11
Orfeo.peerreviewedYes
dc.identifier.doi10.1051/0004-6361/201014124
dc.identifier.scopus2-s2.0-77951807151


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