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S. K. Ballero, Dipartimento di Astronomia, Università di Trieste, Via G. B. Tiepolo 11, I-34124 Trieste, Italy; INAF – Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, I-34121 Trieste, Italy,
F. Matteucci, Dipartimento di Astronomia, Università di Trieste, Via G. B. Tiepolo 11, I-34124 Trieste, Italy; INAF – Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, I-34121 Trieste, Italy,
L. Origlia, INAF – Osservatorio Astronomico di Bologna, Via G. Ranzani 1, I-40127 Bologna, Italy
We present results for the chemical evolution of the Galactic bulge in the context of an inside-out formation model of the Galaxy. A supernovadriven wind was also included in analogy with elliptical galaxies. New observations of chemical-abundance ratios and the metallicity distribution have been employed in order to check the model results. We confirm previous findings that the bulge formed on a very short timescale with quite a high star-formation efficiency and an initial mass function more skewed towards high masses than the one suitable for the Solar neighbourhood. A certain amount of primary nitrogen from massive stars might be required in order to reproduce the nitrogen data at low and intermediate metallicities.
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