LUNALUNA Nucleosintesi stellare (E star ) (E) = S(E)/E e –2 2 cm m m m m Fattore astrofisico Interazioni(stella) (E) (E) dE Picco di Gamow Maxwell Boltzmann.

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LUNALUNA Nucleosintesi stellare (E star ) (E) = S(E)/E e –2 2 cm m m m m Fattore astrofisico Interazioni(stella) (E) (E) dE Picco di Gamow Maxwell Boltzmann Estrap.Mis. Carlo Broggini, INFN-Pd Fattore di Gamow

Laboratory for Underground Nuclear Astrophysics INFN - Laboratori Nazionali del Gran Sasso R.Bonetti, C.Broggini*,F.Confortola, P.Corvisiero, H.Costantini, J. Cruz, A.Formicola, Z. Fülöp, G.Gervino, A.Guglielmetti, C.Gustavino, G. Gyurky, G. Imbriani, A.P.Jesus, M.Junker, A.Lemut, R.Menegazzo, A.Ordine, P.Prati, V.Roca, D.Rogalla, C.Rolfs, M.Romano, C.RossiAlvarez, F.Schümann, O.Straniero, F.Strieder, E. Somorjai, F.Terrasi, H.P.Trautvetter, S.Zavatarelli INFN Sezioni di : Genova, LNGS, Milano, Napoli, Padova e Torino Inst.Physik mit Ionenstrahlen, Ruhr-Universität Bochum (GE) Centro de Fisica Nuclear da Universitade del Lisboa (Portugal) Atomki Debrecen (Hungary)

F = 0.7 m -2 h -1 FnFn cm -2 s -1

LNGS : LUNA2 ( 400 kV) Voltage Range : kV Output Current: 1 mA 75% H 400 kV) 25% H2 : 0.5 mA 4He Absolute Energy error ±300 eV Beam energy spread: <100 eV Long term stability (1 h) : 5 eV Terminal Voltage ripple: 5 Vpp Ge detector LUNA1 ( 50 kV ) Voltage Range : kV Output Current: 1 mA Beam energy spread: 20 eV Long term stability (8 h): 10-4 Terminal Voltage ripple:

pp-chain 99,77% p + p d+ e + + e E 0,42 MeV 0,23% p + e - + p d + e E = 1,44 MeV 3 He + 3 He + 2p 3 He + p + e + + e E 18 MeV ~ % 84,7% 13,8% 0,02%13,78% 3 He + 4 He 7 Be + 7 Be + e - 7 Li + + e E 0,86 MeV 7 Be + p 8 B + d + p 3 He + 7 Li + p + pp I pp III pp II hep hep 8 B 8 Be*+e + + e E 14,06 MeV

3 He ( 3 He,2p) 4 He Q = MeV = 7±2 pb keV) E p max = 10.7 MeV

D(p, g ) 3 He D allequilibrio Vita delle proto-stelle Q=5.5 MeV

14 N(p, g ) 15 O Q=7.3 MeV cno F S 1,14 Eta ammassi globulari S(0)= keV b (Ad98) S(0)= keV b (An99) Alte energie: bersaglio solido + HpGe Basse energie: gas target + BGO E<1.2 MeV E<1.7 MeV

risultati preliminari gamma spectrum of 14 N(p, ) 15 O at Ep=140 keV preliminary S(E) factor ( R/DC->0 transition ) in 14 N(p, ) 15 O results of Schroeder et al.

3 He(, g ) 7 Be Q=1.6 MeV Neutrini solari F Be ~ S 3,4 Studio del Sole F B S 1,7 ~ S(0)=0.53±0.05 keV b (Ad98) S(0)=0.54±0.09 keV b (An99) Termometro del Sole S 34 /S 34 ˜ 3-5% + B / B ~3% Migliore delleliosismologia S 3, ** T 20

25 Mg(p, g ) 26 Al Q=6.3 MeV Nucleosintesi di 24 < A < Mev ( decadimento 26 Al) (da COMPTEL)

(E star ) LUNA ha dimostrato che e possibile misurare Passato: Presente: Futuro: 3 He ( 3 He,2p) 4 He D(p, g ) 3 He dal Sole Proto-stelle 14 N(p, g ) 15 O cno Ammassi globulari 3 He(, g ) 7 Be Sole 25 Mg(p, g ) 26 Al Ciclo Mg-Al Screening Mev