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Prospettive delle attivita' di Astrofisica Nucleare con Recoil Mass Separators

Prospettive delle attivita' di Astrofisica Nucleare con Recoil Mass Separators. Gianluca Imbriani per la collaborazione ERNA. Solar burnings: pp chain. p + p  2 H + e + + n p + e - + p  2 H + e + + n 2 H + p  3 He + g

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Prospettive delle attivita' di Astrofisica Nucleare con Recoil Mass Separators

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  1. Prospettive delle attivita' di Astrofisica Nucleare con Recoil Mass Separators Gianluca Imbriani per la collaborazione ERNA

  2. Solar burnings: pp chain p + p  2H + e+ +np + e- + p  2H + e+ +n 2H + p  3He +g 3He + 3He  4He + 2p 3He + 4He  7Be +g 7Be + e-  7Li +n7Be + p  8B +g 7Li + p  8Be 8B  8Be + e+ +n 8Be  2 4He8Be  2 4He 99.75% 0.25% 86% 14% 99.89% 0.11% CHAIN I CHAIN II CHAIN III Qeff = 26.20 MeV Qeff= 25.66 MeV Qeff= 19.17 MeV Enloss= 2% Enloss= 4% Enloss= 28.3%

  3. (p,g) (p,a) 13C 14N 17O 18F (p,g) 1×109 y (p,g) 2×1012y 10 m e+n e+n 64 s e+n 108 m 13N 15O 17F CN NO 2 m 6×109 y e+n (p,g) (p,g) (p,a) (p,g) 12C 15N 16O 18O (p,a) 1×108 y Solar burnings: CNO cycle

  4. SK+SNO 7 MeV Cl 0.8 MeV Ga 0.2 MeV Neutrino Spectrum Neutrino spectrum To model the Sun we have used FRANEC code (Chieffi and Straniero ApJS 1989) L = 3.844·1033erg·s-1, R = 6.96·1010cm

  5. Dipendenza del flusso di neutrini dai parametri del modello

  6. Incertezze indotte dal modello negli esperimenti

  7. Incertezze indotte dal modello negli esperimenti

  8. Incertezze indotte dal modello negli esperimenti

  9. Jp Ex (keV) 4570 7/2- Q = 1587 keV DC  429 3He+4He DC  0 429 1/2- g Jp Ex (keV) 0 3/2- EC 7Be level scheme g 1/2- 428 3/2- 0 7Li La reazione 3He(4He,g)7Be • Due metodi di misura: • Rivelazione diretta fotoni di cattura; S34(0) = (0.507  0.016) keV b • Misura dell’attività del 7Be impiantato S34(0) = (0.572  0.026) keV b

  10. Caratteristiche cinematiche

  11. Schema dei tempi • Entro la fine del 2003 prime misure di test; • Nel corso del 2004 inizio delle misure della sezione d’urto della 4He(3He,g)7Be.

  12. Prospettive a lungo termine Reazioni con ioni radioattivi appartenenti al biciclo CNO caldo. Astrophysical sites Novae explosion

  13. Nova explosion I First step: Binary sistem between a (CO or ONe) White Dwarf, which accretes mass through the Roche lobe Lagrangian point, and a Red Giant star which accretes it Radius. In the H-rich zone starts the p-p chain.

  14. Nova explosion II Second step: When T  2.4·107 K the CNO cycle starts and nuclear time scale becomes shorter than accretion one; end of accretion phase After about 106 s T  108 K, the convection extends through the original WD material and the actual thermonuclear runaway starts. CNO, NeNa and MgAl extend to the Hot phases enuc = 1.1 ·1016 ergs g-1 s-1

  15. (a,g) (p,a) (p,g) (p,a) 13C 14N 17O 18F 19Ne 20Na (p,g) (p,g) (p,g) e+n e+n 64 s 2 s 18Ne (p,g) 14O 10 m e+n e+n 64 s e+n 108 m 17 s e+n e+n (p,g) 446 ms (p,g) 13N 15O 17F CN NO 2 m e+n (p,g) (p,g) (p,a) (p,g) (p,g) 12C 15N 16O 18O 19F 20Ne (p,g) (p,a) (p,a) Il biciclo CNO esteso

  16. 13N(p,g)14O, 15O(a,g)19Ne, 17F(p,g)18Ne, 18F(p,g)19Ne, 19N(p,g)20Na, 21Na(p,g)22Mg, 22Mg(p,g)23Al, 23Mg(p,g)24Al, 23Al(p,g)24Si For more details see José, Hernanz ApJ 494, 680-690, 1998

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