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Fig. 2


Position of β CMa (cross) and ϵ CMa (asterisk) in the Hertzsprung-Russell diagram in comparison with that of other magnetic stars. The luminosities for the magnetic stars published by Alecian et al. (2014) have been computed on the basis of the stars’ magnitude and distance, the latter given by Alecian et al. (2014). The evolutionary tracks for Milky Way metallicity by Brott et al. (2011) and the evolutionary tracks for solar metallicity by Georgy et al. (2013) are overplotted. Each track is labelled with its initial mass in units of the solar mass. The larger cross on the bottom of the plot shows the size of the median uncertainty in log L/L and Teff, while the smaller cross shows the size of the uncertainties in log L/L and Teff for β CMa and ϵ CMa.

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