J/A+A/XXX/XXXX Stellar models with rotation. 10
=2018A&A...XXXX.XXXX
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ADC_Keywords: Models, evolutionary
Keywords: stars: massive − stars: rotation − stars: interiors −
stars: abundances − stars: chemically peculiar − nuclear reactions,
nucleosynthesis, abundances
Abstract:
Context. Recent studies show that rotation significantly affects the
s-process in massive stars.
Aims. We provide tables of yields for non-rotating and rotating massive
stars between 10 and 150 $M_{\odot}$ at $Z=10^{-3}$ ([Fe/H] $=-1.8$).
Tables for different mass cuts are provided. The complete s-process is
followed during the whole evolution with a network of 737 isotopes,
from Hydrogen to Polonium.
Methods. A grid of stellar models with initial masses of 10, 15, 20, 25,
40, 60, 85, 120 and 150 $M_{\odot}$ and with an initial rotation rate of
both 0 or 40\% of the critical velocity was computed. Three extra models
were computed in order to investigate the effect of faster rotation (70\%
of the critical velocity) and of a lower $^{17}$O($\alpha,\gamma$)
reaction rate.
Results. At the considered metallicity, rotation has a strong impact on
the production of s-elements for initial masses between 20 and
60 $M_{\odot}$. In this range, the first s-process peak is boosted by
$2-3$ dex if rotation is included. Above 60 $M_{\odot}$, s-element
yields of rotating and non-rotating models are similar. Increasing the
initial rotation from 40 \% to 70 \% of the critical velocity enhances
the production of $40 \lesssim Z \lesssim 60$ elements by $\sim 0.5-1$
dex. Adopting a reasonably lower $^{17}$O($\alpha,\gamma$) rate in the
fast rotating model (70 \% of the critical velocity) boosts again the
yields of s-elements with $55 \lesssim Z \lesssim 82$ by about 1 dex.
In particular, a modest amount of Pb is produced. Together with
s-elements, some light elements (particularly fluorine) are strongly
overproduced in rotating models.
Description:
The presented table include the stellar yields of the models of the paper.
The initial masses of the model are 10, 15, 20, 25, 40, 60, 85, 120 and
150 M_sun. The initial rotation rate v_ini / v_crit is either 0, 0.4
or 0.7. Two models (25 M_sun with v_ini / v_crit = 0.7 and 120 M_sun
without rotation) were computed with a 17O(a,g)21Ne reaction rate divided
by ten. For each model, 100 mass cut values are considered (c.f. Sect. 4.2
of the paper for details). Both the ejected mass and the yield (Eq. 3 of
the paper) of the 277 stable (or almost stable) isotopes considered
are given. Ejected mass and yields below 1e-15 in absolute value were
set to zero.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
yields.txt 55 581700 Table of yields
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Byte-by-byte Description of file: yields.txt
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Bytes Format Units Label Explanations
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1- 3 I3 solMass Mass Initial mass
6- 9 F3.1 --- Rot Initial rotation rate (v_ini / v_crit, see text)
12- 13 I1 --- Rate Rate for the 17O(a,g)21Ne reaction (1)
16- 22 F6.2 solMass Mcut Mass cut
24- 29 A5 --- Isotope Isotope name
32- 42 E10.3 solMass Ej Mass Ejected mass of the considered isotope
45- 55 E10.3 solMass Yield Stellar yield (Eq. 3 of the paper)
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Note (1): 0 is for standard rate, 1 means that the rate was divided by 10.
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Acknowledgements:
Arthur Choplin, arthur.choplin(at)unige.ch
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(End) Arthur Choplin [Geneva Obs.]