Blue compact galaxies

Fig. 2. Comparison of N/O ratios for programme stars (filled circles) with the simple models of Meynet Maeder (2002), both including stellar rotation (dotted lines) and with no stellar rotation (dashed lines) and with the analytical models of Henry et al. (2000, solid lines) which were computed to fit the N/O ratios observed in extragalactic HII regions (blue compact galaxies). Empty boxes are metal-rich stars. See Israelian et al. (2004) for details.

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