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New models for the evolution of central stars of planetary nebulae: Faster and Brighter

Published online by Cambridge University Press:  08 August 2017

Marcelo M. Miller Bertolami*
Affiliation:
Instituto de Astrofisica de La Plata, CONICET-UNLP, Paseo del Bosque s/n, (B1900FWA) La Plata, Argentina. email: [email protected]
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Abstract

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The post-asymptotic giant branch (AGB) phase is arguably one of the least understood phases of the evolution of low- and intermediate- mass stars. The recent post-AGB evolutionary sequences computed by Miller Bertolami (2016) are at least three to ten times faster than those previously published by Vassiliadis & Wood (1994) and Blöcker (1995) which have been used in a large number of studies. This is true for the whole mass and metallicity range. The new models are also ~0.1–0.3 dex brighter than the previous models with similar remnant masses. In this short article we comment on the main reasons behind these differences, and discuss possible implications for other studies of post-AGB stars or planetary nebulae.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2017 

References

Abell, G. O. & Goldreich, P., 1966, PASP, 78, 232 CrossRefGoogle Scholar
Althaus, L. G., Córsico, A. H., Kepler, S. O., & Miller Bertolami, M. M., 2008, A&A, 478, 175 Google Scholar
Blöcker, T., 1995, A&A, 299, 755 Google Scholar
Brown, T. M., Smith, E., Ferguson, H. C., et al. 2008, ApJ, 682, 319-335 CrossRefGoogle Scholar
Calcaferro, L. M., Córsico, A. H., & Althaus, L. G., 2016, A&A, 589, A40 Google Scholar
Gesicki, K. & Zijlstra, A. A., 2007, A&A, 467, L29 Google Scholar
Gesicki, K., Zijlstra, A. A., Hajduk, M., & Szyszka, C., 2014, A&A, 566, A48 Google Scholar
Gesicki, K., Zijlstra, A. A., & Miller Bertolami, M. M. 2016, arXiv:1609.08680Google Scholar
Mendez, R. H. 2016, arXiv:1610.08625Google Scholar
Miller Bertolami, M. M., 2016, A&A, 588, A25 Google Scholar
Miller Bertolami, M. M. 2015, in: Dufour, P. and Bergeron, P. & Fontaine, G. (eds.), 19th European Workshop on White Dwarfs, ASP-CS 493, p. 83 Google Scholar
Paczyński, B., 1970, AcA, 20, 47 Google Scholar
Paczyński, B., 1971, AcA, 21, 417 Google Scholar
Schönberner, D., Jacob, R., Steffen, M., & Sandin, C., 2007, A&A, 473, 467 Google Scholar
Shklovsky, I. S. 1957, in: Herbig, G. H. (ed.), Non-stable stars, proceedings from IAU Symposium no. 3, Cambridge University Press, p. 83 Google Scholar
Steffen, M., Schönberner, D., & Warmuth, A., 2008, A&A, 489, 173 Google Scholar
Toalá, J. A. & Arthur, S. J., 2014, MNRAS, 443, 3486 CrossRefGoogle Scholar
Vassiliadis, E. & Wood, P. R., 1994, ApJS, 92, 125 CrossRefGoogle Scholar
Weiss, A. & Ferguson, J. W., 2009, A&A, 508, 1343 Google Scholar