J/A+A/618/A133 Non standard s-process in massive rotating stars (Choplin+, 2018)
Non-standard s-process in massive rotating stars.
Yields of 10-150 M☉ models at Z = 10-3.
Choplin A., Hirschi R., Meynet G., Ekstroem S., Chiappini C., Laird A.
<Astron. Astrophys. 618, A133 (2018)>
=2018A&A...618A.133C 2018A&A...618A.133C (SIMBAD/NED BibCode)
ADC_Keywords: Models, evolutionary ; Abundances
Keywords: stars: massive - stars: rotation - stars: interiors -
stars: abundances - stars: chemically peculiar -
nuclear reactions, nucleosynthesis, abundances
Abstract:
Recent studies show that rotation significantly affects the s-process
in massive stars.
We provide tables of yields for non-rotating and rotating massive
stars between 10 and 150M☉ 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.
A grid of stellar models with initial masses of 10, 15, 20, 25, 40,
60, 85, 120 and 150M☉ 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
17O(α,γ) reaction rate.
At the considered metallicity, rotation has a strong impact on the
production of s-elements for initial masses between 20 and 60M☉.
In this range, the first s-process peak is boosted by 2-3dex if
rotation is included. Above 60M☉, 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≲Z≲60 elements by ∼0.5-1dex. Adopting a reasonably lower
17O(α,γ) rate in the fast rotating model (70% of
the critical velocity) boosts again the yields of s-elements with
55≲Z≲82 by about 1dex. 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 150M☉. The initial rotation rate vini/vcrit is
either 0, 0.4 or 0.7. Two models (25 M_sun with vini /vcrit=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.dat 55 581700 Yields (table4)
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Byte-by-byte Description of file: yields.dat
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Bytes Format Units Label Explanations
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1- 3 I3 Msun Mass Initial mass
(10, 15, 20, 25, 40, 60, 85, 120, 150)
7- 9 F3.1 --- Rot Initial rotation rate (vini/vcrit)
(0.0, 0.4, 0.7)
13 I1 --- Rate [0/1] Rate for the 17O(a,g)21Ne reaction (1)
17- 22 F6.2 Msun Mcut Mass cut
25- 29 A5 --- Isotope Isotope name
33- 42 E10.3 Msun EjMass Ejected mass of the considered isotope
46- 55 E10.3 Msun Yield Stellar yield (Eq. 3 of the paper)
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Note (1): Rate flag as follows:
0 = standard rate
1 = rate was divided by 10
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Acknowledgements:
Arthur Choplin, arthur.choplin(at)unige.ch
(End) Patricia Vannier [CDS] 27-Jul-2018