Effects of metallicity, star formation conditions and evolution of B & Be stars.

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56 , 60 , and 61 , we recover the well-known exact solution of the free convection boundary value problem for the permeable surface when the wall temperature and the

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Ratio of the EW of He i 7065 to He ii 5412 as a function of spectral type for the low-metallicity models calculated in the present study, the solar metallicity models of Martins

With this calibration, and using an aperture photometry of 1" diameter (similar to the seeing of the observations of Yagi et al. For the rest of the sources with no

To derive the respective ZAMS true equatorial velocities we have taken into account four main phenomena determining the variation of the surface rotation with age (Meynet &

We conclude that this star is a carbon-enhanced metal-poor star enriched in elements produced by s-process (CEMP-s), whose enhancement in heavy elements is due to mass transfer from

Note: “Closing” is defined as a positive closure rate horizontally and a positive relative