EDP Sciences
Free Access
Issue
A&A
Volume 569, September 2014
Article Number A45
Number of page(s) 14
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361/201424185
Published online 17 September 2014

Online material

thumbnail Fig. 5

The 84 VLTI/AMBER φdiff measured on Achernar around Brγ at 28 different observing times (format YYYY-MM-DDTHH MM SS) and, for each time, three different projected baselines and baseline position angles, as indicated in the plots. The smooth curves superposed to the observations are the best-fit φdiff obtained without a differential rotation (Domiciano de Souza et al. 2003), gravity-darkened Roche model, as described in Sect. 3. All the observed φdiff points are shown here, knowing that the fit has been performed using all the wavelength points.

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© ESO, 2014

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