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Radial abundance gradients from planetary nebulae and young objects: Age effects

Published online by Cambridge University Press:  30 August 2012

Walter J. Maciel ,
Thaise Rodrigues  and
Roberto Costa
Walter J. Maciel
Affiliation:
Astronomy Department, University of São PauloRua do Matão 1226, 05508-090 São Paulo SP, Brazil email: maciel@astro.iag.usp.br - tsrodrigues@usp.br - roberto@astro.iag.usp.br
Thaise Rodrigues
Affiliation:
Astronomy Department, University of São PauloRua do Matão 1226, 05508-090 São Paulo SP, Brazil email: maciel@astro.iag.usp.br - tsrodrigues@usp.br - roberto@astro.iag.usp.br
Roberto Costa
Affiliation:
Astronomy Department, University of São PauloRua do Matão 1226, 05508-090 São Paulo SP, Brazil email: maciel@astro.iag.usp.br - tsrodrigues@usp.br - roberto@astro.iag.usp.br
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Abstract

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We discuss the effects on the time variation of the gradients resulting from our determinations of the age distributions of CSPN. The main conclusions are: (i) for most CSPN with accurate radial velocities the kinematic ages are usually under 3 Gyr, so that the differences between the gradients of these objects and of younger objects are expected to be small; (ii) results based on age-metallicity relations suggest that there is an older PN population for which the gradients are steeper, in agreement with open cluster data.

Keywords

planetary nebulae: generalGalaxy: abundancesGalaxy: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S283: Planetary Nebulae: An Eye to the Future , July 2011 , pp. 424 - 425
Copyright
Copyright © International Astronomical Union 2012

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