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2.5. Stellar Mg abundances in the Galactic center

  • S. V. Ramirez (a1), K. Sellgren (a1), D. M. Terndrup (a1), J. S. Carr (a1), S. Balachandran (a1) and R. D. Blum (a1)...

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Star formation in the Galactic Center (GC) happens under unusual conditions, which include high gas temperatures, high velocity dispersions, and strong tidal shear (Spergel & Blitz 1992; Blitz et al. 1993). All these conditions may lead to an initial mass function (IMF) dominated by massive stars (Morris & Serabyn 1996). A history of chemical evolution dominated by massive stars is expected to result in enhancements of α-elements (Mg, Si, Ca, Ti) relative to Fe (Wheeler et al. 1989). This argument is the main motivation to study the abundance of Fe and Mg in GC stars.

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References

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Blitz, L., Binney, J., Lo, K. Y., Bally, J., & Ho, P. T. P. 1993, Nature, 361, 417.
Blum, R. D., Sellgren, K., & DePoy, D. L. 1996, AJ, 112, 1988.
Brown, J. A., Johnson, H. R., Alexander, D. R., Cutright, L. C., & Sharp, C. M. 1989, ApJS, 71, 623.
Carr, J. S., Sellgren, K., & Balachandran, S. 1996a, in The Galactic Center, 4th CTIO/ESO Workshop, PASP Conf. Ser. 102, ed. Gredel, R., p. 212.
Carr, J. S., Sellgren, K., & Balachandran, S. 1996b, in 9th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, ed. Pallavicini, R. & Dupree, A. K., p. 711.
Kleinmann, S. G. & Hall, D. N. B. 1986, ApJS, 62, 501.
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Sellgren, K., Carr, J. S., & Balachandran, S., presented at IAU Symp. 184, The Central Regions of the Galaxy and Galaxies, August 1997, Kyoto, Japan.
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2.5. Stellar Mg abundances in the Galactic center

  • S. V. Ramirez (a1), K. Sellgren (a1), D. M. Terndrup (a1), J. S. Carr (a1), S. Balachandran (a1) and R. D. Blum (a1)...

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