000004538 001__ 4538
000004538 005__ 20200131165058.0
000004538 0247_ $$2DOI$$a10.25518/0037-9565.8694
000004538 037__ $$aSCART-2020-0012
000004538 037__ $$aSCART-2019-0111
000004538 100__ $$aLampens, P.
000004538 245__ $$aEclipse mapping of Algol-type systems with oscillating delta Scuti type components
000004538 260__ $$c2019
000004538 500__ $$ain Proceedings of the second Belgo-Indian Network for Astronomy & Astrophysics (BINA) workshop "BINA as an expanding international collaboration" (09-12/10/2018, Brussels, Belgium)
000004538 520__ $$aThe oscillating Algol-type (oEA) stars are the former secondaries of evolved, semi-detached eclipsing binaries which are (still) undergoing mass transfer and form a newly detected class of pulsators close to the main sequence. Their unique feature consists of mass accretion onto the atmosphere of the pulsating star. Mass accretion affects the mass, radius, density as well as the star\u2019s evolution. Such stars are therefore very attractive targets for asteroseismic studies. A new tool for mode identification of pulsating components in eclipsing binaries consists in using the event of primary eclipse as a spatial filter to resolve the pulsations across the stellar surface of the pulsator. During an eclipse, depending on the spatial structure of modes represented by the wave numbers (l,m), different shapes of the pulsation amplitude and phase variations can be observed. A comparison between the modelled and the observed amplitudes and phases then provides the correct mode identification. The method needs a geometrical model, the pulsation frequencies and the light curves as input. The geometrical model can be obtained from a simultaneous modelling of the light and radial velocity curves. The pulsation frequencies are obtained from subtracting a binary model from the original light curves followed by a frequency analysis of the residuals. We will identify and illustrate systems where observations with a fast CCD camera equipping the 3.6-m DOT telescope could deliver the data needed for the application of the eclipse mapping method.
000004538 594__ $$aNO
000004538 6531_ $$astars, eclipsing binaries, fundamental parameters, accretion, Delta Scuti
000004538 700__ $$aVermeylen, L.
000004538 700__ $$aDe Cat, P.
000004538 700__ $$aVan Cauteren, P.
000004538 773__ $$c89-94$$nOctober 2019$$pBulletin de la Société Royale des Sciences de Liège$$v88$$y2019
000004538 8560_ $$fpatricia.lampens@observatoire.be
000004538 905__ $$apublished in
000004538 980__ $$aREFERD