J/ApJ/769/99 Nucleosynthetic yields for stars >12M☉ (Brown+, 2013)
Nucleosynthetic constraints on the mass of the heaviest supernovae.
Brown J.M., Woosley S.E.
<Astrophys. J., 769, 99 (2013)>
=2013ApJ...769...99B 2013ApJ...769...99B
ADC_Keywords: Models ; Supernovae ; Abundances
Keywords: galaxies: abundances; hydrodynamics; supernovae: general;
nuclear reactions, nucleosynthesis, abundances; stars: abundances
Abstract:
We explore the sensitivity of nucleosynthesis in massive stars to the
truncation of supernova explosions above a certain mass. It is assumed
that stars of all masses contribute to nucleosynthesis by their
pre-explosive winds, but above a certain limiting main sequence mass,
MBH, the presupernova star becomes a black hole and ejects nothing
more. The solar abundances from oxygen to atomic mass 90 are fit quite
well assuming no cutoff at all, i.e., by assuming all stars up to
120M☉ make successful supernovae. Little degradation in the fit
occurs if MBH is reduced to 25M☉. If this limit is reduced
further however, the nucleosynthesis of the s-process declines
precipitously and the production of species made in the winds, e.g.,
carbon, becomes unacceptably large compared with elements made in the
explosion, e.g., silicon and oxygen. By varying uncertain physics,
especially the mass loss rate for massive stars and the rate for the
22Ne(α,n)25Mg reaction rate, acceptable nucleosynthesis
might still be achieved with a cutoff as low as 18M☉. This would
require, however, a supernova frequency three times greater than the
fiducial value obtained when all stars explode in order to produce the
required 16O. The effects of varying MBH on the nucleosynthesis of
60Fe and 26Al, the production of helium as measured by
ΔY/ΔZ, and the average masses of compact remnants are also
examined.
Description:
The yield tables of Woosley & Heger (2007PhR...442..269W 2007PhR...442..269W) give the
nucleosynthesis of all species from hydrogen through lead for
supernovae resulting from non-rotating massive stars with solar
metallicity for the following initial masses: 12-33 (every integer
mass), 35-60 (every 5 masses), 60-80 (every 10 masses), 100, and
120 solar masses. The authors calculated explosions for four sets of
models parameterized by the mass cut and explosion energy. Here we use
their standard set for which the explosion energy was 1.2x1051erg
and the mass cut was located at the "entropy jump" where S/NAk=4.0.
These are their "A" models.
The values of some key species are provided in Table 1. Using this
grid of nucleosynthetic yields, we constructed a stellar population
using the high-end initial mass function described by Reid & Wilson
(2006ApJ...650..970R 2006ApJ...650..970R). See section 2 for further explanations.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 180 64 Yields table for 12≤M/M☉≤120
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See also:
J/A+A/566/A146 : Pair-instability supernovae models (Kozyreva+, 2014)
J/A+A/558/A131 : Model spectra of hot stars at the pre-SN stage (Groh+, 2013)
J/ApJS/199/38 : Presupernova evolution (Limongi+, 2012)
J/ApJ/724/341 : Nucleosynthesis of massive metal-free stars (Heger+, 2010)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- Model Model type (1)
8- 10 I3 Msun Mass [12/120] Initial model mass
12- 20 E9.3 Msun H [0/36] The H yield
22- 30 E9.3 Msun He [0.05/64] The He yield
32- 40 E9.3 Msun C [0.002/11] The C yield
42- 50 E9.3 Msun N [0/0.6] The N yield
52- 60 E9.3 Msun O [0.007/8] The O yield
62- 70 E9.3 Msun Ne [0.001/2] The Ne yield
72- 80 E9.3 Msun Mg [0.0007/0.5] The Mg yield
82- 90 E9.3 Msun Si [0.0008/0.5] The Si yield
92-100 E9.3 Msun S [0.0004/0.3] The S yield
102-110 E9.3 Msun Ar [0.0001/0.06] The Ar yield
112-120 E9.3 Msun Ca The Ca yield
122-130 E9.3 Msun Ge70 The 70Ge yield
132-140 E9.3 Msun Se76 The 76Se yield
142-150 E9.3 Msun Sr86 The 86Sr yield
152-160 E9.3 Msun Sr87 The 87Sr yield
162-170 E9.3 Msun Al26 The 26Al yield
172-180 E9.3 Msun Fe60 The 60Fe yield
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Note (1): Model type (see the "Description" section above):
SN = The "A" supernova explosion model
(Woosley & Heger 2007PhR...442..269W 2007PhR...442..269W).
pre-SN = The "A" presupernova winds model
(Woosley & Heger 2007PhR...442..269W 2007PhR...442..269W).
See the Description section above.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 15-Dec-2014