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- W71843903 abstract "Abstract. We have computed the photometric magnitudes ofrotating atmospheres–based on the simple model of Collins–fora grid suitable for main-sequence and slightly evolved stars ofspectral type A0 to F5. A gravity-darkening law valid for radia-tive and convective envelopes has been considered. The generalresults are given as magnitude differences between rotating andnon-rotating copartners to allow for the use of any photomet-ric calibration. A simple interpolation on these results gives thephotometric parameters for interior rotating models but we alsoindicate how they can be used to correct for the effect of rota-tion when an investigation with non-rotating models is carriedout. We illustrate the procedure with the interesting case of thePraesepe Cluster.Key words: stars: rotation – stars: fundamental parameters –stars: variables: δ Sct – Galaxy: open clusters and associations:individual: Praesepe1. IntroductionThisarticledealswiththerelationbetweenglobalparametersoffast rotating F and A stars and their photometric parameters. Itwas first conceived in the framework of the asteroseismology ofδ Scuti stars. In particular, in a recent work, Michel et al. (1999)and Hern´andez et al. (1998) analysed several δ Scuti stars in thePraesepe Cluster and attempted to obtain information on suchstars from their modes of oscillation. As in other works, it wasclear that the seismological analysis must be accompanied bythe most accurate possible estimates of the stellar parameters.Since most of these stars are fast rotators, this is not a simpletask and, as shown by Michel et al. (1998, 1999), the inclusionof the photometric effect of rotation on the location of the starsinthecolour–magnitudediagramcanbynomeansbeneglected.A method for computing the emergent flux from a rapidlyrotating star was given by Collins (1963). Some important im-provements were developed by Collins (1965, 1966), Hardorp& Strittmatter (1968) and Maeder & Peytremann (1970, 1972).The latter authors included spectral lines in their atmosphericmodels, developing the most consistent calculations up to thattime. Michel et al. (1999) used the results of Maeder & Peytre-" @default.
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- W71843903 date "1999-06-01" @default.
- W71843903 modified "2023-10-18" @default.
- W71843903 title "PHOTOMETRIC PARAMETERS FOR ROTATING MODELS OF A- AND F-TYPE STARS" @default.
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