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Titolo: Weak proton capture on He3  art. no. 015801
Autore: Marcucci, LE; Schiavilla, R; Viviani, M; Kievsky, A; Rosati, S; Beacom, JF;
 Indirizzi:
 Old Dominion Univ, Dept Phys, Norfolk, VA 23529 USA Old Dominion Univ Norfolk VA USA 23529 , Dept Phys, Norfolk, VA 23529 USA Jefferson Lab, Newport News, VA 23606 USA Jefferson Lab Newport News VA USA 23606 n Lab, Newport News, VA 23606 USA Ist Nazl Fis Nucl, Sez Pisa, I56100 Pisa, Italy Ist Nazl Fis Nucl Pisa Italy I56100 Nucl, Sez Pisa, I56100 Pisa, Italy Univ Pisa, Dept Phys, I56100 Pisa, Italy Univ Pisa Pisa Italy I56100Univ Pisa, Dept Phys, I56100 Pisa, Italy CALTECH, Phys Dept 161 33, Pasadena, CA 91125 USA CALTECH Pasadena CA USA91125 H, Phys Dept 161 33, Pasadena, CA 91125 USA
 Titolo Testata:
 PHYSICAL REVIEW C
fascicolo: 1,
volume: 6301,
anno: 2001,
pagine: 5801 
 SICI:
 05562813(200101)6301:1<5801:WPCOH>2.0.ZU;22
 Fonte:
 ISI
 Lingua:
 ENG
 Soggetto:
 NEUTRINO ENERGYSPECTRUM; MONTECARLO CALCULATIONS; FEWBODY NUCLEI; CROSSSECTION; FORMFACTORS; HEPNEUTRINOS; BETADECAY; POLARIZATION OBSERVABLES; ELECTRONSCATTERING; MESONIC ENHANCEMENT;
 Tipo documento:
 Article
 Natura:
 Periodico
 Settore Disciplinare:
 Physical, Chemical & Earth Sciences
 discip_EC
 Citazioni:
 91
 Recensione:
 Indirizzi per estratti:
 Indirizzo: Marcucci, LE Univ Pisa, Dept Phys, I56100 Pisa, Italy Univ Pisa Pisa Italy I56100 Dept Phys, I56100 Pisa, Italy



 Citazione:
 L.E. Marcucci et al., "Weak proton capture on He3  art. no. 015801", PHYS REV C, 6301(1), 2001, pp. 5801
Abstract
The astrophysical S factor for the proton weak capture on He3 is calculated with correlatedhypersphericalharmonics bound and continuum wave functions corresponding to realistic Hamiltonians consisting of the Argonne nu (14) or Argonne nu (18) twonucleon and UrbanaVIII or UrbanaIX threenucleon interactions. The nuclear weak charge and current operators have vector and axialvector components that include one and manybody terms. All possible multipole transitions connecting any of the pHe3 S and Pwave channels to the He4 bound state are considered. The S factor at a pHe3 centerofmass energy of 10 keV, close to the Gamowpeak energy, is predicted to be 10.1 x 10(20) keV b with the AV18/UIX Hamiltonian, a factor of similar or equal to1.5 larger than the value adopted in the standard solar model. The Pwave transitions are found to be important, contributing about 40% of the calculated S factor. The energy dependence is rather weak: the AV18/UIX zeroenergy S factor is 9.64 x 10(20) keV b, only 5% smaller than the 10 keV result quoted above. The model dependence is also found to be weak: the zeroenergy S factor is calculated to be 10.2 x 10(20) keV b with the older AV14/UVIII model, only 6% larger than the AV18/UIX result. Our best estimate for the S factor at 10 keV is therefore (10.1+/0.6) x 10(20) keV b, when the theoretical uncertainty due to the model dependence is included. This value for the calculated S factor is not as large as determined in fits to the SuperKamiokande data in which the hrp flux normalization is free. However, the precise calculation of the S factor and the consequent absoluteprediction for the hrp neutrino flux will allow much greater discrimination among proposed solar neutrino oscillation solutions.
ASDD Area Sistemi Dipartimentali e Documentali, Università di Bologna, Catalogo delle riviste ed altri periodici
Documento generato il 08/04/20 alle ore 08:40:02