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Titolo:
REACTION-RATES FOR O-18(ALPHA,GAMMA)NE-22, NE-22(ALPHA,GAMMA)MG-26, AND NE-22(ALPHA,N)MG-25 IN STELLAR HELIUM BURNING AND S-PROCESS NUCLEOSYNTHESIS IN MASSIVE STARS
Autore:
KAPPELER F; WIESCHER M; GIESEN U; GORRES J; BARAFFE I; ELEID M; RAITERI CM; BUSSO M; GALLINO R; LIMONGI M; CHIEFFI A;
Indirizzi:
KERNFORSCHUNGSZENTRUM KARLSRUHE GMBH,INST KERNPHYS,POB 3640 D-76021 KARLSRUHE GERMANY UNIV NOTRE DAME,DEPT PHYS NOTRE DAME IN 46556 UNIV STERNWARTE GOTTINGEN D-37083 GOTTINGEN GERMANY OSSERV ASTRON TORINO I-10025 PINO TORINESE ITALY UNIV TURIN,IST FIS GEN I-10125 TURIN ITALY CNR,IST ASTROFIS SPAZIALE I-00044 FRASCATI ITALY
Titolo Testata:
The Astrophysical journal
fascicolo: 1, volume: 437, anno: 1994,
parte:, 1
pagine: 396 - 409
SICI:
0004-637X(1994)437:1<396:RFONA>2.0.ZU;2-Y
Fonte:
ISI
Lingua:
ENG
Soggetto:
BETA-DECAY RATES; NEUTRON-CAPTURE; LOW ENERGIES; EVOLUTION; C-12(ALPHA,GAMMA)O-16; METALLICITY; ISOCHRONES; RESONANCES; PHASES; TABLES;
Keywords:
NUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCES; STARS, EARLY-TYPE; STARS, INTERIORS;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Science Citation Index Expanded
Citazioni:
54
Recensione:
Indirizzi per estratti:
Citazione:
F. Kappeler et al., "REACTION-RATES FOR O-18(ALPHA,GAMMA)NE-22, NE-22(ALPHA,GAMMA)MG-26, AND NE-22(ALPHA,N)MG-25 IN STELLAR HELIUM BURNING AND S-PROCESS NUCLEOSYNTHESIS IN MASSIVE STARS", The Astrophysical journal, 437(1), 1994, pp. 396-409

Abstract

New experimental results in O-18(Li-6, d) and Ne-22(Li-6, d) alpha transfer reaction studies have been utilized to calculate the resonance strength of low-energy resonances in the alpha-capture on O-18 and Ne-22. The present results imply a significant increase of the reaction rates for O-18(alpha, gamma)Ne-22 and Ne-22(alpha, gamma)Mg-26. The Ne-22(alpha, n)Mg-25 rate might be strongly enhanced by a possible resonance at 633 keV. The respective uncertainties are presented as a function of temperature. The influence of the proposed reaction rates on thes-process nucleosynthesis during core helium burning has been investigated in the range 15 < M/M(circle dot) < 30. The resulting uncertainties are compared to those related to the modeling of core helium burning in massive stars. This comparison indicates that the s-process may be a useful constraint for the evolution and convection in massive stars, provided the persistent problem of the 633 keV resonance in the Ne-22(alpha, n)Mg-25 channel can be solved.

ASDD Area Sistemi Dipartimentali e Documentali, Università di Bologna, Catalogo delle riviste ed altri periodici
Documento generato il 04/12/20 alle ore 12:28:46