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Titolo:
RADIATIVE C-13 BURNING IN ASYMPTOTIC GIANT BRANCH STARS AND S-PROCESSING
Autore:
STRANIERO O; GALLINO R; BUSSO M; CHIEFFI A; RAITERI CM; LIMONGI M; SALARIS M;
Indirizzi:
OSSERV COLLURANIA I-64100 TERAMO ITALY UNIV TURIN,IST FIS GEN I-10125 TURIN ITALY OSSERV ASTRON TORINO I-10025 PINO TORINESE ITALY CNR,IST ASTROFIS SPAZIALE I-00044 FRASCATI ITALY OSSERV ASTRON ROMA I-00040 MONTE PORZIO CATO ITALY CNR,IST ASTROFIS SPAZIALE ROME ITALY UNIV ROME,IST ASTRON ROME ITALY
Titolo Testata:
The Astrophysical journal
fascicolo: 2, volume: 440, anno: 1995,
parte:, 2
pagine: 85 - 87
SICI:
0004-637X(1995)440:2<85:RCBIAG>2.0.ZU;2-I
Fonte:
ISI
Lingua:
ENG
Soggetto:
LOW-MASS STARS; SMALL CORE MASS; PROCESS NUCLEOSYNTHESIS; CARBON STAR; THERMAL PULSES; EVOLUTION; ISOTOPES; MODELS;
Keywords:
NUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCES; STARS, AGB AND POST-AGB; STARS, EVOLUTION;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Science Citation Index Expanded
Citazioni:
25
Recensione:
Indirizzi per estratti:
Citazione:
O. Straniero et al., "RADIATIVE C-13 BURNING IN ASYMPTOTIC GIANT BRANCH STARS AND S-PROCESSING", The Astrophysical journal, 440(2), 1995, pp. 85-87

Abstract

We present new evolutionary calculations for a 3 M. star of Population I starting from the zero-age main sequence and followed up to the 25th thermal pulse of the asymptotic giant branch. The third dredge-up is found to occur in a self-consistent way from the 14th pulse on. We show that any amount of C-13 possibly synthesized at the H/He interfaceduring the interpulse period is completely burnt through (alpha, n) reactions before the next pulse develops. As a consequence, s-elements are produced in a radiative environment, at a neutron density of at most a few 10(7) n cm(-3). They are then engulfed and diluted into the next convective pulse, where a second (minor) neutron burst occurs, driven by the Ne-22(alpha, n)Mg-25 reaction marginally activated near theend of the He-shell instability. Despite the differences of the present model with respect to past calculations, we predict s-process distributions very close to those computed by allowing C-13 to burn in convective pulses: C-13 burning and the ensuing s-processing are confirmedto account for the main observational and experimental constraints. The reasons for this are briefly discussed. Since no C-13 survives the interpulse phase, we conclude that no modifications of the pulse shapedue to the energy feedback from the C-13(alpha, n)O-16 reaction occur.

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Documento generato il 04/12/20 alle ore 13:05:11