000002052 001__ 2052
000002052 005__ 20160701171657.0
000002052 0247_ $$2DOI$$a10.1051/0004-6361:20053051
000002052 037__ $$aASTROimport-209
000002052 100__ $$aZorec, J.
000002052 245__ $$aOn the evolutionary status of Be stars. I. Field Be stars near the Sun
000002052 260__ $$c2005
000002052 520__ $$aA sample of 97 galactic field Be stars were studied by taking into account the effects induced by the fast rotation on their fundamental parameters. All program stars were observed in the BCD spectrophotometric system in order to minimize the perturbations produced by the circumstellar environment on the spectral photospheric signatures. This is one of the first attempts at determining stellar masses and ages by simultaneously using model atmospheres and evolutionary tracks, both calculated for rotating objects. The stellar ages (τ) normalized to the respective inferred time that each rotating star can spend in the main sequence phase (τ_MS) reveal a mass-dependent trend. This trend shows that: a) there are Be stars spread over the whole interval 0 ⪉ τ/τ_MS ⪉ 1 of the main sequence evolutionary phase; b) the distribution of points in the (τ/τMS,M/M⊙) diagram indicates that in massive stars (M ⪆ 12~M⊙) the Be phenomenon is present at smaller τ/τ_MS age ratios than for less massive stars (M ⪉ 12~M⊙). This distribution can be due to: i) higher mass-loss rates in massive objets, which can act to reduce the surface fast rotation; ii) circulation time scales to transport angular momentum from the core to the surface, which are longer the lower the stellar mass. 
000002052 700__ $$a Frémat, Y.
000002052 700__ $$a Cidale, L.
000002052 773__ $$c235-248$$i1$$pAstronomy and Astrophysics$$v441$$y2005
000002052 85642 $$ahttp://esoads.eso.org/abs/2005A%26A...441..235Z
000002052 905__ $$apublished in
000002052 980__ $$aREFERD