dc.contributor |
Universitat Politècnica de Catalunya. Departament de Física Aplicada |
dc.contributor |
Universitat Politècnica de Catalunya. DF - Dinàmica No Lineal de Fluids |
dc.contributor.author |
Doherty, Carolyn L. |
dc.contributor.author |
Siess, Lionel |
dc.contributor.author |
Lattanzio, John |
dc.contributor.author |
Gil Pons, Pilar |
dc.date |
2010-01-01 |
dc.identifier.citation |
Doherty, C. [et al.]. Super asymptotic giant branch stars. I - Evolution code comparison. "Monthly notices of the Royal Astronomical Society", 01 Gener 2010, vol. 401, p. 1453-1464. |
dc.identifier.citation |
0035-8711 |
dc.identifier.uri |
http://hdl.handle.net/2117/9195 |
dc.language.iso |
eng |
dc.rights |
Attribution-NonCommercial-NoDerivs 3.0 Spain |
dc.rights |
info:eu-repo/semantics/openAccess |
dc.rights |
http://creativecommons.org/licenses/by-nc-nd/3.0/es/ |
dc.subject |
Àrees temàtiques de la UPC::Aeronàutica i espai |
dc.subject |
Nuclear reactions |
dc.subject |
Nucleosynthesis |
dc.subject |
Asymptotic giant branch stars |
dc.subject |
Estels |
dc.title |
Super asymptotic giant branch stars. I - Evolution code comparison |
dc.type |
info:eu-repo/semantics/publishedVersion |
dc.type |
info:eu-repo/semantics/article |
dc.description.abstract |
We present an extensive set of detailed stellar models in the mass range 7.7–10.5M over the
metallicity range Z = 10−5–0.02. These models were produced using the Monash University
version of the Mount Stromlo Stellar Structure Program (MONSTAR) and follow the evolution
from the pre-main sequence to the first thermal pulse of these super asymptotic giant branch
stars. A quantitative comparison is made to the study of Siess. Prior to this study, only
qualitative comparisons and code validations existed in this critical mass range, and the
large variations in the literature were largely unexplained. The comparison presented here
is particularly detailed due to the standardization of the input physics, where possible. The
minimum initial mass of star which ignites carbon, Mup, was found to agree within 0.2M
between the codes over the entire metallicity range.We find exceptional agreement in the model
results between these two codes for all stages of evolution up to and including carbon burning.
For additional comparison, we also present results from the EVOLVE code, a modified version of
the IBEN code as described in Gil-Pons, Guti´errez & Garc´ıa-Berro for some important variables
during the carbon burning phase. Several numerical tests showed that the carbon burning
phase is weakly dependent on the spatial resolution but that inadequate temporal resolution
alters the behaviour of the convective zones.We also discovered that stars just below Mup may
experience a carbon flash that is not followed by the development of the flame. Such aborted
carbon burning models thus preserve a CO core surrounding by a 0.2–0.3M shell of partially
burnt carbon material. We present a simplified algorithm for calculating carbon burning that
only relies on tracking two species, 12C and 16O, but which tests show works quite accurately
for the a wide range of initial masses and compositions |
dc.description.abstract |
Peer Reviewed |