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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

References

Andreuzzi, G., Bragaglia, A., Tosi, M., & Marconi, G., 2011, MNRAS, 412, 1265 Google Scholar
Daflon, S. & Cunha, K., 2004, ApJ, 617, 1115 CrossRefGoogle Scholar
Durand, S., Acker, A., & Zijlstra, A., 1998, A&AS, 132, 13 Google Scholar
Holmberg, J., Nordström, B., & Andersen, J., 2007, A&A, 475, 519 Google Scholar
Holmberg, J., Nordström, B., & Andersen, J., 2009, A&A, 501, 941 Google Scholar
Luck, R. E., Andrievsky, S. M., Kovtyukh, V. V., et al. , 2011, AJ, 142, 51 CrossRefGoogle Scholar
Maciel, W. J. & Costa, R. D. D., 2009, IAU Symp. 254, Electronic publication, CUP Google Scholar
Maciel, W. J., Costa, R. D. D., & Idiart, T. E. P., 2010, A&A, 512, A19 Google Scholar
Maciel, W. J., Rodrigues, T. S., & Costa, R. D. D., 2011, Rev. Mexicana A&A, 47, 401 Google Scholar
Magrini, L., Stanghellini, L., & Villaver, E., 2009, ApJ, 696, 729 CrossRefGoogle Scholar
Nordström, B., Mayor, M., Andersen, J. et al. , 2004, A&A, 418, 989 Google Scholar
Stanghellini, L., Magrini, L., Villaver, E., & Galli, D., 2010, A&A, 521, A3 Google Scholar