J/A+A/566/A146 Pair-instability supernovae models (Kozyreva+, 2014)
Explosion and nucleosynthesis of low redshift pair instability supernovae.
Kozyreva A., Yoon S.-C., Langer N.
<Astron. Astrophys. 566, A146 (2014)>
=2014A&A...566A.146K 2014A&A...566A.146K
ADC_Keywords: Models ; Supernovae ; Abundances
Keywords: nuclear reactions, nucleosynthesis, abundances - stars: evolution -
stars: massive - supernovae: general - stars: abundances
Abstract:
Both recent observations and stellar evolution models suggest that
pair-instability supernovae (PISNe) could occur in the local Universe,
at metallicities below Z☉/3. Previous PISN models were mostly
produced at very low metallicities in the context of the early
Universe.
We present new PISNe models at a metallicity of Z=0.001, which are
relevant for the local Universe.
We take the self-consistent stellar evolutionary models of
pair-instability progenitors with initial masses of 150 and 250 solar
masses at metallicity of Z=0.001 by Langer et al.
(2007A&A...475L..19L 2007A&A...475L..19L) and follow the evolution of these models through
the supernova explosions, using a hydrodynamics stellar evolution code
with an extensive nuclear network including 200 isotopes. Both models
explode as PISNe without leaving a compact stellar remnant. Our models
produce a nucleosynthetic pattern that is generally similar to that of
Population III PISN models, which is mainly characterized by the
production of large amounts of elements and a strong deficiency of the
odd-charged elements. However, the odd-even effect in our models is
significantly weaker than that found in Population III models. The
comparison with the nucleosynthetic yields from core-collapse
supernovae at a similar metallicity (Z=0.002) indicates that PISNe
could have strongly influenced the chemical evolution below Z=0.002,
assuming a standard initial mass function. The odd-even effect is
predicted to be most prominent for the intermediate mass elements
between silicon and calcium. With future observations of chemical
abundances in Population II stars, our result can be used to constrain
the number of PISNe that occurred during the past evolution of our
Galaxy.
Description:
Table 3: Total nucleosynthetic yields in solar masses and production
factors for 150 (150M) and 250 (250M) solar masses PISN models at
metallicity Z=0.001. Yields include matter lost by the stellar wind
and decay products.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 56 80 Total nucleosynthetic yields and production factors
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See also:
J/ApJ/664/1033 : Variations in supernova yields (Young+ 2007)
J/MNRAS/408/827 : Simulations of supernova explosions (Dessart+, 2010)
J/A+A/558/A131 : Model spectra of hot stars at the pre-SN stage (Groh+, 2013)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- El Element name
3- 5 I3 --- A [1/71] Isotope number
9- 17 E9.3 Msun Y(150) Isotopic yields for model 150M
22- 30 E9.3 Msun Y(250) Isotopic yields for model 250M
35- 43 E9.3 --- PF(150) Isotopic production factors for model 150M
48- 56 E9.3 --- PF(250) Isotopic production factors for model 250M
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Acknowledgements:
Alexandra Kozyreva, kozyreva(at)astro.uni-bonn.de
(End) Patricia Vannier [CDS] 30-May-2014