Issue |
A&A
Volume 497, Number 2, April II 2009
|
|
---|---|---|
Page(s) | 463 - 468 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361/200811362 | |
Published online | 05 March 2009 |
Thermohaline mixing in super-AGB stars
1
Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles (ULB), CP 226, 1050 Brussels, Belgium e-mail: siess@astro.ulb.ac.be
2
Centre for Stellar and Planetary Astrophysics, School of Mathematical Sciences, Monash University, Victoria 3800, Australia
Received:
17
November
2008
Accepted:
26
January
2009
Aims. We present the first study of the effects of thermohaline mixing on the
structure and evolution of solar-composition super-AGB (SAGB) stars in
the mass range
.
Methods. We developed and analyzed stellar models taking into account thermohaline mixing and varying mixing efficiencies.
Results. In SAGB stars, thermohaline mixing becomes important after carbon has
been ignited off-center and it affects significantly the propagation of the
flame.
In the radiative layers located below the convective
carbon-burning zone, a molecular weight inversion is created which allows
the efficient transport of chemicals. The outward diffusion of
12C
from the CO-rich core into the flame, depletes the burning front of fuel
and causes the extinction of the flame before it reaches the center. As a
consequence the amount of unburnt carbon can be as high as in
mass at the center of the star. During the subsequent thermally
pulsing SAGB phase, the high temperature at the base of the
convective envelope prevents the development of thermohaline
instabilities associated with 3He burning as
found in low-mass red giant stars.
Conclusions. In contrast to the case of low-mass RGB stars, thermohaline mixing is unable to alter the surface composition of SAGB stars. We also emphasize that if the SAGB star evolves into an electron-capture supernovae, the 12C remaining in the core may alter the hydrodynamical explosion and modify the explosive nucleosynthesis.
Key words: stars: evolution / stars: supernovae: general / nuclear reactions, nucleosynthesis, abundances / instabilities
© ESO, 2009
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