1. Nuclear Burning in Stars (E star ) ( E ) = S(E) e –2 E -1 Reaction Rate(star) (E) (E) dE Gamow Peak Maxwell Boltzmann Extrap.Meas. LUNA results Men in pits or wells sometimes see the stars…. Aristotle Carlo Broggini, INFN-Pd

2. INFN - Laboratori Nazionali del Gran Sasso D.Bemmerer,R.Bonetti,C.Broggini*,F. Confortola,P.Corvisiero,H.Costantini,Z.Elekes, A.Formicola, Z. Fülöp, G.Gervino,A.Guglielmetti, C.Gustavino, G. Gyurky, G. Imbriani, M.Junker, A.Lemut, B.Limata, V.Lozza,M.Marta,R.Menegazzo, P.Prati, V.Roca, C.Rolfs, M.Romano, C.RossiAlvarez, O.Straniero,F.Strieder, E.Somorjai,F.Terrasi,H.P.Trautvetter INFN : Genova, LNGS, Milano, Napoli, Padova, Torino Inst.Physik mit Ionenstrahlen, Ruhr- Universität Bochum (GE) Atomki Debrecen (Hungary) LUNA

3. luna Voltage Range :50-400 kV Output Current: 1 mA (@ 400 kV) Absolute Energy error ±300 eV Beam energy spread: <100 eV Long term stability (1 h) : 5 eV Terminal Voltage ripple: 5 Vpp Ge detector F = 0.7 m -2 h -1 FnFn 3 10 -6 cm -2 s -1

4. p + p d + e + + e d + p 3 He + 3 He + 3 He +2p 3 He + 4 He 7 Be + 7 Be+e - 7 Li + + e 7 Be + p 8 B + 7 Li + p 8 B 2 + e + + e 84.7 %13.8 % 13.78 % 0.02% pp chain

5. 14 N(p, g ) 15 O Q=7.3 MeV - 504 -21 278 14 N+p 7297 7556 7276 6859 6793 6176 5241 5183 0 15 O 1/2 + 7/2 + 5/2 + 3/2 + 3/2 - 5/2 + 1/2 + 1/2 -

6. 10 -7 mbar10 -6 mbar10 -4 mbar 0.5-2 mbar Windowless gas-target Max 10 mbar Low energy: gas target + BGO

7. Reaction Rate = 10.95 0.83 counts/day Background rate = 21.14 0.75 counts/day t = 49.12 daysQ = 927 7 C beam energy: 80 keV

8. cno from the Sun Globular cluster age C yield in AGB stars S t (0)=1.61±0.08±0.16 keV b

9. 3 He(, g ) 7 Be Solar Neutrinos: 7 Be, 8 B BBN 7 Li prompt gammaCross section from prompt gamma down to 90 keV (CM energy) using 4 He beam on 3 He target radioactive decayActivation via off-line radioactive decay measurements of the 7 Be atoms collected in the beam catcher All with a final error < 5 % Q=1.6 MeV

10. Summary of previous measurements = 0.51 ± 0.02 keV b = 0.57 ± 0.03 keV b 0.53 ± 0.05 keV b (9%) [Adelberger 98] 0.54 ± 0.09 keV b (16%) [NACRE 99] Recommended S 34 (0) values: R-matrix analysis: 0.51 ± 0.04 keV b (8%) [Descouvemont 2004]

13. Activation measurement o 4 He beam @ 350 keV o ~ 230 µA oRecirculated 3 He @ 0.7 mbar 478 214 Bi 7 Be

14. SourceDeterminationRelative Uncertainty Detector efficiencyMeasured1.8 % Beam currentCalibrated calorimeter1.5 % Beam heating effectMeasured (typical correction: 5%) 1.3 % Target thicknessPressure and temperature measurements 0.6 % Backscattering lossMeasured and simulated (typical correction: 2.1%) 0.5 % 478 keV -ray branchingFrom literature0.4 % Incomplete 7 Be collectionMeasured and simulated (typical correction: 1.6%) 0.4% Effective energyMeasured0.5-0.8 % Parasitic 7 Be productionMeasured upper limit0.04 % Sputtering lossUpper limit from MC Simulation0.02 % Total3.0 % Systematic uncertainties and corrections

17. Prompt -spectra o 4 He beam @ 400 keV o ~ 300 µA oIrradiation time: 4.4d o 4 He beam @ 220 keV o ~ 240 µA oIrradiation time: 24.4d

18. 3 He(, g ) 7 Be: the Sun: 7 Be and 8 B neutrinos Big-Bang 7 Li 14 N(p, g ) 15 O: down to 70 keV (T=60 T 6 ) cno from the Sun reduced by 2 Globular cluster age increased by 0.7-1 Gy Higher C yield in AGB stars LUNA has shown that it is possible to measure (E star ): 3 He ( 3 He,2p) 4 He, 2 H(p, g ) 3 He 3 He ( 3 He,2p) 4 He: down to 16 keV no resonance within the solar Gamow Peak

20. S 14,1 /5 S 14,1 x5 Standard CF88

22. 25 Mg(p, g ) 26 Al Q=6.3 MeV Nucleosynthesis Mg-Al Astronomical interest of the from 26 Al decay Ge detectorsCross section at 180-400 keV (CM energy) using Ge detectors (not underground) BGO summing crystalsCross section at lower energies using BGO summing crystals (underground)