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Convective overshooting and production of s-nuclei in massive stars during their core He-burning phase | | M. L. Pumo
; G. Contino
; A. Bonanno
; R. A. Zappalá
; | | Date: |
27 Sep 2010 | | Abstract: | In this research note we analyze the role of convective overshooting on the
production of s-nuclei in massive stars during their core He-burning phase.
Using the "post-processing" technique, we explore the role of the convective
overshooting on the production of s-nuclei in stellar models of different
initial mass and metallicity ($15 leq M_{ZAMS}/M_{odot} leq 25$; $10^{-4}
leq Z leq 0.02$), considering a range of values for the parameter $f$ which
determines the overall efficiency of convective overshooting. We find
enhancements in the production of s-nuclei until a factor $sim 6$ (measured as
the average overproduction factor of the 6 s-only nuclear species with
$60lesssim Alesssim90$) in all our models of different initial mass and
metallicity having $f$ in the range $0.01-0.035$ (i.e. models with
overshooting), compared to the production obtained with "no-overshooting"
models (i.e. models having the same initial mass and metallicity but
$f=10^{-5}$). Moreover the results indicate that the link between the
overhooting parameter $f$ and the s-process efficiency is essentially monotonic
in all our models of different initial mass and metallicity. Also evident is
the higher s-process efficiency when, for a given f value, we progressively
increase both the mass of the models from 15 M$_odot$ to 25 M$_odot$ and the
Z value from 10$^{-4}$ to 0.02. The possible consequences of these results on
some open questions linked to the s-process weak component efficiency, as well
as a "rule of thumb" to evaluate the impact of the convective overshooting on
the yields of a generation of stars, are also briefly discussed. | | Source: | arXiv, 1009.5333 | | Services: | Forum | Review | PDF | Favorites | |
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