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J/ApJ/787/10    Solar s-process contributions with GCE model   (Bisterzo+, 2014)

Galactic chemical evolution and solar s-process abundances: dependence on the 13C-pocket structure. Bisterzo S., Travaglio C., Gallino R., Wiescher M., Kappeler F. <Astrophys. J., 787, 10 (2014)> =2014ApJ...787...10B (SIMBAD/NED BibCode)
ADC_Keywords: Models, evolutionary ; Sun ; Abundances ; Solar system Keywords: stars: AGB and post-AGB - Galaxy: evolution - Sun: abundances Abstract: We study the s-process abundances (A≳90) at the epoch of the solar system formation. Asymptotic giant branch yields are computed with an updated neutron capture network and updated initial solar abundances. We confirm our previous results obtained with a Galactic chemical evolution (GCE) model: (1) as suggested by the s-process spread observed in disk stars and in presolar meteoritic SiC grains, a weighted average of s-process strengths is needed to reproduce the solar s distribution of isotopes with A>130; and (2) an additional contribution (of about 25%) is required in order to represent the solar s-process abundances of isotopes from A=90 to 130. Furthermore, we investigate the effect of different internal structures of the 13C pocket, which may affect the efficiency of the 13C(α,n)16O reaction, the major neutron source of the s process. First, keeping the same 13C profile adopted so far, we modify by a factor of two the mass involved in the pocket; second, we assume a flat 13C profile in the pocket, and we test again the effects of the variation of the mass of the pocket. We find that GCE s predictions at the epoch of the solar system formation marginally depend on the size and shape of the 13C pocket once a different weighted range of 13C-pocket strengths is assumed. We obtain that, independently of the internal structure of the 13C pocket, the missing solar system s-process contribution in the range from A=90 to 130 remains essentially the same. Description: The general structure of the GCE model adopted in this work is the same described by Travaglio et al. (2004ApJ...601..864T). The GCE model follows the composition of stars, stellar remnants, interstellar matter (atomic and molecular gas), and their mutual interaction, in the three main zones of the Galaxy, halo, thick disk, and thin disk. We concentrate on the chemical evolution inside the solar annulus, located 8.5 kpc from the Galactic center. The thin disk is divided into independent concentric annuli, and we neglect any dependence on Galactocentric radius. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 76 207 Solar s-process contributions for isotopes from Kr to Bi obtained with GCE model
See also: J/MNRAS/418/284 : s-process in low-metallicity stars. II. (Bisterzo+, 2011) J/A+A/586/A49 : r- and s- process elements in Milky Way disk (Battistini+, 2016) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 7 A7 --- Isotope Isotope identifier 9 A1 --- f_Isotope [bc] Flag on Isotope (1) 11- 15 F5.1 % Main-s Bisterzo et al. (2011, J/MNRAS/418/284) main-s contribution (2) 17 A1 --- f_Main-s [cd] Flag on Main-s (3) 19- 22 F4.1 % e_Main-s ? Uncertainty in Main-s (4) 24- 29 F6.2 % T04-LMS Travaglio et al. (2004ApJ...601..864T) LMS Solar s-process distribution 31 A1 --- f_T04-LMS [d] Flag on T04-LMS (3) 33- 37 F5.2 % T04-IMS Travaglio et al. (2004ApJ...601..864T) IMS Solar s-process distribution 39- 43 F5.1 % T04+ Travaglio et al. (2004ApJ...601..864T) LMS+IMS Solar s-process distribution 45- 46 A2 --- f_T04+ [cd ] Flag on T04+ (3) 47- 49 F3.1 % e_T04+ ? Uncertainty in T04+ (4) 51- 55 F5.2 % TW-LMS This work LMS Solar s-process distribution 57 A1 --- f_TW-LMS [cd] Flag on LMS (3) 59- 62 F4.2 % TW-IMS This work IMS Solar s-process distribution 64- 69 F6.2 % TW+ This work LMS+IMS Solar s-process distribution 71 A1 --- f_TW+ [d] Flag on TW+ (3) 73- 76 F4.1 % e_TW+ ? Uncertainty in TW+ (4)
Note (1): Flag as follows: b = Note that massive stars may produce a consistent amount of Kr-Rb-Sr-Y-Zr, and in minor quantity up to Te-Xe (Pignatari et al. 2010ApJ...710.1557P; 2013ApJ...762...31P). c = An isotope that receives an additional contribution from p-process (Travaglio et al. 2011ApJ...739...93T). Note (2): The main-s component, which is reproduced as an average between AGB models of M=1.5 and 3 M and half solar metallicity, as in Arlandini et al. (1999ApJ...525..886A), is also listed for comparison. Note (3): Flag as follows: c = Overabundance with respect to solar (in percentage). d = Percentages include the s-contribution (≤1%) by r-only isotopes not included in this table (124Sn, 130Te, 136Xe, 150Nd). Note (4): Uncertainties refer to solar abundances by Anders & Grevesse (1989GeCoA..53..197A; T04+) and Lodders et al. (2009, LanB, 4, 44; Main-s and TW+).
History: From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 03-Aug-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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