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Chemical Analysis of B stars within 9–11 kpc from the Galactic Center

Published online by Cambridge University Press:  09 March 2010

Maria Isela Zevallos Herencia  and
Simone Daflon
Maria Isela Zevallos Herencia
Affiliation:
Observat'orio Nacional, Rua General José Cristino 77, CEP:20921.400, São Cristóvão, Rio de Janeiro, Brazil email: [email protected];[email protected]
Simone Daflon
Affiliation:
Observat'orio Nacional, Rua General José Cristino 77, CEP:20921.400, São Cristóvão, Rio de Janeiro, Brazil email: [email protected];[email protected]
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Abstract

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Radial gradients of metallicity are supported by observations of different young objects in the Galactic thin disk. The shape of the abundance distributions, however, is not completely constrained. Some works describe the abundance distributions as a function of the Galactocentric distance RG by linear fits with a single slope. On the other hand some analyses of open clusters, cepheids and OB stars suggest a discontinuity in the abundance distributions around RG=10 kpc. In this work we analyse a sample of 13 B stars members of four open clusters located within RG=9-11 kpc in order to better constrain the chemical distribution in this region of the disk.

Keywords

abundancesearly-type stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S265: Chemical Abundances in the Universe: Connecting First Stars to Planets , August 2009 , pp. 362 - 363
Copyright
Copyright © International Astronomical Union 2010

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