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J/A+A/524/A45  Overproduction factors of s-nuclei in massive stars (Pumo+, 2010)

Convective overshooting and production of s-nuclei in massive stars during their core He-burning phase. Pumo M.L., Contino G., Bonanno A., Zappala R.A. <Astron. Astrophys. 524, A45 (2010)> =2010A&A...524A..45P
ADC_Keywords: Models, evolutionary ; Stars, normal ; Stars, metal-deficient ; Abundances Keywords: nuclear reactions, nucleosynthesis, abundances - convection - stars: evolution - stars: interiors Abstract: Using the "post-processing" technique, we explore the role of the convective overshooting on the production of s-nuclei in stellar models of different initial mass and metallicity (MZAMS in the range 15-25M Z in the range 10-4-0.02), considering a range of values for the parameter f, which determines the overall efficiency of convective overshooting. We find enhancements in the production of s-nuclei until a factor ∼6 (measured as the average overproduction factor of the 6 s-only nuclear species with 60<A<90) in all our models of different initial mass and metallicity having f in the range 0.01-0.035 (i.e. models with overshooting), compared to the production obtained with "no-overshooting" models (i.e. models having the same initial mass and metallicity but f=10-5). Moreover the results indicate that the link between the overshooting parameter f and the s-process efficiency is essentially monotonic in all our models of different initial mass and metallicity. Also evident is the higher s-process efficiency when, for a given f value, we progressively increase both the mass of the models from 15 to 25M and the Z value from 10-4 to 0.02. Description: We present the overproduction factors of the 49 s-nuclei having mass number A in the range 69-209, for all our models of different initial mass, initial metallicity and f value. The values obtained by The, El Eid & Meyer (2007ApJ...655.1058T) for their Z=0.02 stellar models with a similar mass and input physics are also reported in tablea4.dat for comparison. All the data refer to the end of the core He-burning phase. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea4.dat 135 49 Overproduction factors for all the models with initial metallicity Z=0.02 tablea5.dat 125 49 Overproduction factors for all the M=20M models with initial metallicity Z<0.02
See also: VI/109 : Population Synthesis Models at very low metallicities (Schaerer, 2003) VI/118 : Stellar Models until He burning (Claret+ 1995-1998) Byte-by-byte Description of file: tablea4.dat
Bytes Format Units Label Explanations
1- 3 I3 --- A [69/209] Mass number 4- 5 A2 --- El Nuclide (chemical) symbol 8- 15 E8.3 --- M15T07 ? Overproduction factors obtained by The, El Eid & Meyer (2007ApJ...655.1058T) for their Z=0.02, M=15M stellar model (G1) 18- 25 E8.3 --- M15f.001 Overproduction factors for our Z=0.02, M=15M stellar model with overshooting parameter f=0.00001 (G1) 28- 35 E8.3 --- M15f1 Overproduction factors for our Z=0.02, M=15M stellar model with overshooting parameter f=0.01 (G1) 38- 45 E8.3 --- M15f2 Overproduction factors for our Z=0.02, M=15M stellar model with overshooting parameter f=0.02 (G1) 48- 55 E8.3 --- M15f3.5 Overproduction factors for our Z=0.02, M=15M stellar model with overshooting parameter f=0.035 (G1) 58- 65 E8.3 --- M20T07 ? Overproduction factors obtained by The, El Eid & Meyer (2007ApJ...655.1058T) for their Z=0.02, M=20M stellar model (G1) 68- 75 E8.3 --- M20f0001 Overproduction factors for our Z=0.02, M=20M stellar model with overshooting parameter f=0.00001 (G1) 78- 85 E8.3 --- M20f1 Overproduction factors for our Z=0.02, M=20M stellar model with overshooting parameter f=0.01 (G1) 88- 95 E8.3 --- M20f2 Overproduction factors for our Z=0.02, M=20M stellar model with overshooting parameter f=0.02 (G1) 98-105 E8.3 --- M20f3.5 Overproduction factors for our Z=0.02, M=20M stellar model with overshooting parameter f=0.035 (G1) 108-115 E8.3 --- M25T07 ? Overproduction factors obtained by The, El Eid & Meyer (2007ApJ...655.1058T) for their Z=0.02, M=25M stellar model (G1) 118-125 E8.3 --- M25f.001 Overproduction factors for our Z=0.02, M=25M stellar model with overshooting parameter f=0.00001 (G1) 128-135 E8.3 --- M25f1 Overproduction factors for our Z=0.02, M=25M stellar model with overshooting parameter f=0.01 (G1)
Byte-by-byte Description of file: tablea5.dat
Bytes Format Units Label Explanations
1- 3 I3 --- A [69/209] Mass number 4- 5 A2 --- El Nuclide (chemical) symbol 8- 15 E8.3 --- M20Z.01f.001 Overproduction factors for our Z=0.0001, M=20M stellar model with overshooting parameter f=0.00001 (G1) 18- 25 E8.3 --- M20Z.01f1 Overproduction factors for our Z=0.0001, M=20M stellar model with overshooting parameter f=0.01 (G1) 28- 35 E8.3 --- M20Z.01f2 Overproduction factors for our Z=0.0001, M=20M stellar model with overshooting parameter f=0.02 (G1) 38- 45 E8.3 --- M20Z.01f3.5 Overproduction factors for our Z=0.0001, M=20M stellar model with overshooting parameter f=0.035 (G1) 48- 55 E8.3 --- M20Z.5f.001 Overproduction factors for our Z=0.005, M=20M stellar model with overshooting parameter f=0.00001 (G1) 58- 65 E8.3 --- M20Z.5f1 Overproduction factors for our Z=0.005, M=20M stellar model with overshooting parameter f=0.01 (G1) 68- 75 E8.3 --- M20Z.5f2 Overproduction factors for our Z=0.005, M=20M stellar model with overshooting parameter f=0.02 (G1) 78- 85 E8.3 --- M20Z.5f3.5 Overproduction factors for our Z=0.005, M=20M stellar model with overshooting parameter f=0.035 (G1) 88- 95 E8.3 --- M20Z1f.001 Overproduction factors for our Z=0.01, M=20M stellar model with overshooting parameter f=0.00001 (G1) 98-105 E8.3 --- M20Z1f1 Overproduction factors for our Z=0.01, M=20M stellar model with overshooting parameter f=0.01 (G1) 108-115 E8.3 --- M20Z1f2 Overproduction factors for our Z=0.01, M=20M stellar model with overshooting parameter f=0.02 (G1) 118-125 E8.3 --- M20Z1f3.5 Overproduction factors for our Z=0.01, M=20M stellar model with overshooting parameter f=0.035 (G1)
Global Notes: Note (G1): the overproduction factor of a nuclid is the ratio of mass fractions of s-only nucleus at the end of s-process, to the initial mass fraction of the same nucleus (see section 4 of the paper for details)
Acknowledgements: Maria Letizia Pumo, mlpumo(at)oact.inaf.it
(End) Maria Letizia Pumo [INAF-OACt, Italy], Patricia Vannier [CDS] 26-Oct-2010
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