SIMBAD references

We present the results of statistical analyses of a sample of 627 Be stars. The parameters of intrinsic polarization (p_*), projected rotational velocity (v sin i), and near IR excesses have been investigated. The values of p_* have been estimated for a much larger and more representative sample of Be stars (≃490 objects) than previously. We have confirmed that most Be stars of early spectral type have statistically larger values of polarization and IR excesses in comparison with the late spectral type stars. It is found that the distributions of p_* diverge considerably for the different spectral subgroups. In contrast to late spectral types (B5-B9.5), the distribution of p_* for B0-B2 stars does not peak at the value p_*=0%. Statistically significant differences in the mean projected rotational velocities (<vsini>) are found for different spectral subgroups of Be stars in the sense that late spectral type stars (V luminosity class) generally rotate faster than early types, in agreement with previously published results. This behaviour is, however, not obvious for the III-IV luminosity class stars. Nevertheless, the calculated values of the ratio v_t/v_c of the true rotational velocity, v_t, to the critical velocity for break-up, v_c, is larger for late spectral type stars of all luminosity classes. Thus, late spectral type stars appear to rotate closer to their break-up rotational velocity. The distribution of near IR excesses for early spectral subgroups is bi-modal, the position of the second peak displaying a maximum value E(V-L)≃1.3mag for O-B1.5 stars, decreasing to E(V-L)≃0.8mag for intermediate spectral types (B3-B5). It is shown that bi-modality disappears for late spectral types (B6-B9.5). No correlations were found between p_* and near IR excesses and between E(V-L) and vsini for the different subgroups of Be stars. In contrast to near IR excesses, a relation between p_* and far IR excesses at 12 µm is clearly seen. A clear relation between p_* and vsini (as well as between p_* and <vsini>/v_c) is found by the fact that plots of these parameters are bounded by a ``triangular" distribution of p_*:vsini, with a decrease of p_* towards very small and very large vsini (and <vsini>/v_c) values. The latter behaviour can be understood in the context of a larger oblateness of circumstellar disks for the stars with a rapid rotation. From the analysis of correlations between different observational parameters we conclude that circumstellar envelopes for the majority of Be stars are optically thin disks with the range of the half-opening angle of 10°<Θ<40°.