L. Carigi* and M. Peimbert**
Instituto de Astronomía, Universidad Nacional Autónoma de México. Apdo. Postal 70–264, México 04510, D.F., México (* carigi@astroscu.unam.mx, ** peimbert@astroscu.unam.mx).
Received 2010 November 18
Accepted 2011 February 3
RESUMEN
]]> Presentamos modelos de evolución química del disco galáctico con diferentes rendimientos dependientes de Z. Encontramos que una tasa moderada de pérdida de masa en estrellas masivas de metalicidad solar produce un excelente ajuste con los gradientes de C/H y C/O del disco de la Galaxia. El mejor modelo reproduce: las abundancias de H, He, C y O derivadas de líneas de recombinación en M17, las abundancias protosolares y las relaciones C/O–O/H, C/Fe–Fe/H y O/Fe–Fe/H derivadas de estrellas de la vecindad solar. La concordancia del modelo con las abundancias protosolares implica que el Sol se originó a una distancia galactocéntrica similar a la actual. El modelo para r = 3 kpc implica que una fracción de las estrellas en la dirección del bulbo se formó en el disco interno. Nuestro modelo reproduce la relación C/O–O/H derivada de regiones H II extragalácticas en galaxias espirales.
ABSTRACT
We present chemical evolution models of the Galactic disk with different Z dependent yields. We find that a moderate mass loss rate for massive stars of solar metallicity produces an excellent fit to the observed C/H and C/O gradients of the Galactic disk. The best model also fits: the H, He, C, and O abundances derived from recombination lines of M17, the protosolar abundances, and the C/O–O/H, C/Fe–Fe/H, and O/Fe–Fe/H relations derived from solar vicinity stars. The agreement of the model with the protosolar abundances implies that the Sun originated at a Galactocentric distance similar to the one it has now. Our model for r = 3 kpc implies that a fraction of the stars in the direction of the bulge formed in the inner disc. We obtain a good agreement between our model and the C/O versus O/H relationship derived from extragalactic H II regions in spiral galaxies.
Key Words: galaxies: abundances — galaxies: evolution — Galaxy: bulge — H II regions — ISM: abundances — Sun: abundances.
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ACKNOWLEDGMENTS
We thank Jorge García–Rojas and César Esteban for useful discussions. We are also grateful to the anonymous referee for a careful reading of the manuscript and many excellent suggestions. This work was partly supported by the Conacyt grants 60354 and 129753.
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