The Wayback Machine - https://web.archive.org/web/20160202032755/http://adsabs.harvard.edu/abs/2006A&A...448..717S
Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· References in the article
· Citations to the Article (130) (Citation History)
· Refereed Citations to the Article
· Associated Articles
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Evolution of massive AGB stars. I. Carbon burning phase
Authors:
Siess, L.
Affiliation:
AA(Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles, CP 226, 1050 Brussels, Belgium )
Publication:
Astronomy and Astrophysics, Volume 448, Issue 2, March III 2006, pp.717-729 (A&A; Homepage)
Publication Date:
03/2006
Origin:
EDP Sciences
Astronomy Keywords:
stars: evolution, nuclear reactions, nucleosynthesis, , abundances, stars: AGB and post-AGB
DOI:
10.1051/0004-6361:20053043
Bibliographic Code:
2006A&A...448..717S

Abstract

We present new computations of the evolution of solar metallicity stars in the mass range 9 - 12 M&sun;. This first paper of a series focuses on the propagation of the carbon burning flame front and provides a detailed analysis of the structural evolution up to the formation of the neon-oxygen core. Our calculations which do not include overshooting indicate that off-center carbon ignition is restricted to a small mass range between 9.0 and 11.3 M&sun;. The chemical imprints of the first and second dredge-ups on the surface composition are analyzed and compared to "standard" less massive stars. It results that, aside from being more luminous and slightly bluer in the HR diagram, massive AGB stars are almost indistinguishable from their lower mass counterparts, as far as the chemical composition is concerned. During the second dredge-up, we note however that the envelope penetrates deeper into the He burning shell than lower mass stars. Our simulations indicate that above 11.0 M&sun;, the depth of the second dredge up is considerably reduced, marking the transition between low and massive stars. We also investigate the effects of the nuclear uncertainties associated with 12{{C}} + 12{{C}} reactions and show that it has a little impact on the core composition. Finally we describe the nucleosynthesis and chemical structure of the newly formed neon-oxygen core.

Associated Articles

Part  1     Part  2     Part  3    

Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
  New!

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints
    


Morty Proxy This is a proxified and sanitized view of the page, visit original site.