J/ApJ/854/18 Nucleosynthesis of p nuclides (Travaglio+, 2018)
Role of core-collapse supernovae in explaining solar system abundances of p
nuclides.
Travaglio C., Rauscher T., Heger A., Pignatari M., West C.
<Astrophys. J., 854, 18 (2018)>
=2018ApJ...854...18T 2018ApJ...854...18T
ADC_Keywords: Atomic physics; Supernovae; Stars, masses; Abundances; Models
Keywords: Galaxy: abundances ; Galaxy: evolution ;
nuclear reactions, nucleosynthesis, abundances ; supernovae: general
Abstract:
The production of the heavy stable proton-rich isotopes between 74Se
and 196Hg-the p nuclides-is due to the contribution from different
nucleosynthesis processes, activated in different types of stars.
Whereas these processes have been subject to various studies, their
relative contributions to Galactic chemical evolution (GCE) are still
a matter of debate. Here we investigate for the first time the
nucleosynthesis of p nuclides in GCE by including metallicity and
progenitor mass-dependent yields of core-collapse supernovae (ccSNe)
into a chemical evolution model. We used a grid of metallicities and
progenitor masses from two different sets of stellar yields and
followed the contribution of ccSNe to the Galactic abundances as a
function of time. In combination with previous studies on p-nucleus
production in thermonuclear supernovae (SNIa), and using the same GCE
description, this allows us to compare the respective roles of SNeIa
and ccSNe in the production of p-nuclei in the Galaxy. The γ
process in ccSN is very efficient for a wide range of progenitor
masses (13M☉-25M☉) at solar metallicity. Since it is a
secondary process with its efficiency depending on the initial
abundance of heavy elements, its contribution is strongly reduced
below solar metallicity. This makes it challenging to explain the
inventory of the p nuclides in the solar system by the contribution
from ccSNe alone. In particular, we find that ccSNe contribute less
than 10% of the solar p nuclide abundances, with only a few
exceptions. Due to the uncertain contribution from other
nucleosynthesis sites in ccSNe, such as neutrino winds or α-rich
freeze out, we conclude that the light p-nuclides 74Se, 78Kr,
84Sr, and 92Mo may either still be completely or only partially
produced in ccSNe. The γ-process accounts for up to twice the
relative solar abundances for 74Se in one set of stellar models and
196Hg in the other set. The solar abundance of the heaviest p
nucleus 196Hg is reproduced within uncertainties in one set of our
models due to photodisintegration of the Pb isotopes 208,207,206Pb.
For all other p nuclides, abundances as low as 2% of the solar level
were obtained.
Description:
In this work, we use non-rotating stellar models of C. West & A. Heger
(2018, in preparation) computed with the KEPLER stellar evolution,
nucleosynthesis, and SN code (Weaver+ 1978ApJ...225.1021W 1978ApJ...225.1021W ; Rauscher+
2002ApJ...576..323R 2002ApJ...576..323R). The progenitor models were calculated using the
physics setup, opacities, and nuclear reaction rates as described in
Woosley & Heger (2007PhR...442..269W 2007PhR...442..269W) and in West+ (2013ApJ...769....2W 2013ApJ...769....2W).
The nucleosynthetic yields for seven different initial masses, from
13M☉ to 30M☉, and 14 different metallicities, from
Z=1.5x10-6 up to Z=0.3 were calculated. The initial composition of
the models used the Galactic Chemical History model of West & Heger
(J/ApJ/774/75), which is based on Lodders+ (2009LanB...4B..712L 2009LanB...4B..712L) solar
abundances.
Details of KEPLER models will be published in a forthcoming paper
(C. West & A. Heger 2018, in preparation), including the impact of
choosing proper metallicity-dependent initial compositions. See
section 2 for further explanations.
The second set of p-nuclide yields used in this work are taken from
Pignatari+ (NuGrid; 2016, J/ApJS/225/24). The one-dimensional stellar
progenitors were calculated using the stellar evolution code GENEC
(Eggenberger+ 2008Ap&SS.316...43E 2008Ap&SS.316...43E) for massive stars.
See section 3 for further explanations.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 169 259 *KEPLER xi45 ccSN model: ejected mass
table2.dat 40 111 *NUGRID ccSN model: ejected mass
table3.dat 67 35 *Chemical evolution of p-nuclei with KEPLER and
NUGRID models
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Note on table1.dat, table2.dat and table3.dat:
See the "Description" section above for the KEPLER and NuGrid references.
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See also:
J/ApJ/724/341 : Nucleosynthesis of massive metal-free stars (Heger+, 2010)
J/ApJ/726/25 : Production of the p-process nuclei in SNe Ia (Kusakabe+, 2011)
J/MNRAS/412/1441 : SNe luminosity functions (Li+, 2011)
J/ApJS/199/38 : Presupernova evolution (Limongi+, 2012)
J/ApJ/774/75 : Solar isotopic decomposition for nucleosynthesis (West+, 2013)
J/ApJS/225/24 : NuGrid stellar data set I. Yields (H to Bi) (Pignatari+, 2016)
J/ApJS/237/13 : 13-120M☉ massive stars models & yields (Limongi+, 2018)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 Msun Mass [13/30] Initial mass
4- 13 A10 --- Iso Nuclide/Mass Number
15- 25 E11.6 Msun MF01 [2.8e-10/80.6] Mass Fraction at Z=2.425e-02
27- 37 E11.6 Msun MF02 [2.2e-10/83.8] Mass Fraction at Z=1.930e-02
39- 49 E11.6 Msun MF03 [2.1e-10/83.4] Mass Fraction at Z=1.530e-02
51- 61 E11.6 Msun MF04 [1.4e-10/88.1] Mass Fraction at Z=9.655e-03
63- 73 E11.6 Msun MF05 [8.7e-11/91.2] Mass Fraction at Z=6.092e-03
75- 85 E11.6 Msun MF06 [5.5e-11/86.8] Mass Fraction at Z=3.844e-03
87- 97 E11.6 Msun MF07 [1.2e-12/60.7] Mass Fraction at Z=2.425e-03
99-109 E11.6 Msun MF08 [3.4e-13/60.9] Mass Fraction at Z=1.530e-03
111-121 E11.6 Msun MF09 [2.9e-14/60.7] Mass Fraction at Z=4.839e-04
123-133 E11.6 Msun MF10 [3.6e-15/63.1] Mass Fraction at Z=1.530e-04
135-145 E11.6 Msun MF11 [4.5e-16/61.6] Mass Fraction at Z=4.839e-05
147-157 E11.6 Msun MF12 [5.6e-17/59.6] Mass Fraction at Z=1.530e-05
159-169 E11.6 Msun MF13 [6.4e-14/88] Mass Fraction at Z=1.530e-06
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 Msun Mass [15/25] Initial mass
4- 10 A7 --- Iso Isotope
12- 20 E9.4 Msun MF01 [1.5e-12/1.3] Mass Fraction at Z=2.00e-02
22- 30 E9.4 Msun MF02 [7.3e-13/1.5] Mass Fraction at Z=1.00e-02
32- 40 E9.4 Msun MF03 [1.4e-12/0.4]? Mass Fraction at Z=2.00e-02 r2
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Iso Isotope
9- 17 A9 --- Sol Solar system composition by
Lodders+ 2009LanB...4B..712L 2009LanB...4B..712L
19- 27 A9 --- xi45 Galactic chemical evolution results using
yields from the xi45 KEPLER model
29- 37 A9 --- xi25 Galactic chemical evolution results using
yields from the xi25 KEPLER model
39- 47 A9 --- nocutoff Galactic chemical evolution results using
yields from the nocutoff KEPLER model
49- 57 A9 --- ertl Galactic chemical evolution results using
yields from the ertl KEPLER model
59- 67 A9 --- Nugrid Galactic chemical evolution results using
yields from the NUGRID model
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 07-Nov-2018