1.  ( E ) = S(E) e –2   E -1 2      m  m   m   m   Reaction Rate(star)    (E)  (E) dE Gamow Peak  Maxwell Boltzmann Extrap. Meas.  Carlo Broggini INFN-Padova Stellar Energy+Nucleosynthesis  (E star ) with E star << E Coulomb Hydrogen Burning LUNA, the Sun and the other stars S(E)

2. Laboratory for Underground Nuclear Astrophysics Beam: H,He Voltage Range :50-400 kV Output Current: ~1 mA Absolute Energy error ±300 eV Beam energy spread: <100 eV Long term stability (1 h) : 5 eV Terminal Voltage ripple: 5 Vpp Ge detector

3. Resonance? Hydrogen burning in the Sun @15*10 6 degrees: 6*10 11 kg/s of H He +0.7% M H E activation=prompt gamma  at low energy with 4% error H+ 2 H burning in proto-stars @10 6 degrees

4. 3 He ( 3 He,2p) 4 He Q = 12.86 MeV E p max = 10.7 MeV Suppression of 7 Be and 8 B e due to a resonance?  min =20 fb (2 events/month) No resonance at the Gamow peak Neutrino oscillations

5. 14 N(p, g ) 15 O Q=7.3 MeV cno F  S 1,14 Globular Cluster Age S(0)=3.5 -1.6 +0.4 keV b (Ad98) S(0)=3.2 -0.8 +0.8 keV b (An99) Age Cluster =F( £ turnoff ) £ to =F(S 1,14 ) RedBlue turnoff £ Surface colour

6. - 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 - “High” energy: solid target + HpGe gamma spectrum of 14 N(p,  ) 15 O at 140 keV beam energy 14 N(p, g ) 15 O Low energy: gas target + BGO beam energy 90 keV

7. * ½ cno from the Sun * Globular Cluster age +1Gy * more C at the surface of AGB From a measurement of cno from the Sun S t (0)=1.57±0.13 keV b Metallicity of the Sun core (C+N) Photosphere and core metallicity equal? Solar composition problem: Z/X ~0.024 ~ 0.018 SSM predictions disagree with Helioseismology results cno =f(Z,S 14 ), ~30% decrease from high to low metallicity

8. 2 H(α, g ) 6 Li Q=1.47 MeV 15 N(p, g ) 16 O Q=12.13 MeV 17 O(p, g ) 18 F Q=5.6 MeV 23 Na(p, g ) 24 Mg Q=11.7 MeV 22 Ne(p, g ) 23 Na Q=8.8 MeV 18 O(p, g ) 19 F Q=8.0 MeV 25 Mg(p, g ) 26 Al Q=6.3 MeV LUNA beyond the Sun: isotope production in the hydrogen burning shell of AGB stars (~30-100 T 6 ), Nova nucleosynthesis (~100-500 T 6 ) and BBN............ 17 O(p, α ) 14 N Q=1.2 MeV 18 O(p, α ) 15 N Q=4.0 MeV

9. 12 C( , g ) 16 O the most important reaction of nuclear astrophysics: production of the elements heavier than A=16, star evolution from He burning to the explosive phase and ratio C/O 13 C( ,n) 16 O, 22 Ne( ,n) 25 Mg the stellar sources of the neutrons responsible for the S-process ( , g ) on 14 N, 15 N, 18 O…… LUNA beyond the Hydrogen burning: 3.5 MV accelerator mainly devoted to Helium-Burning (in stars: ~ 100 T 6, ~10 5 gr/cm 3 ) June 2012: accelerator+site preparation financed by the Italian Ministry of University and Research with 2.8 ME ‘Starting the LUNA-MV Collaboration’, LNGS, February 6th-8th 2013

10. 3 He( , g ) 7 Be: 14 N(p, g ) 15 O:   down to 70 keV cno reduced by  2 with 8% error Sun core metallicity Globular cluster age increased by 0.7-1 Gy More carbon at the surface of AGB stars 3 He ( 3 He,2p) 4 He:  down to 16 keV no resonance within the solar Gamow Peak Cross section measured with 4% error 7 Be ≈ prompt g 25 Mg(p, g ) 26 Al: first measurement of the 92 keV resonance, strength ωγ =(2.9±0.6)x 10 -10 eV 15 N(p, g ) 16 O:   down to 70 keV, reduced by  2 Future: Hydrogen and Helium burning (3.5 MV accelerator) 17 O(p, g ) 18 F: rate uncertainty @ Novae temperature reduced to 5% uncertainty on 18 O, 18 F and 19 F less than 10% (from 40-50%)

12. 3 He( , g ) 7 Be Solar Neutrinos: 7 Be, 8 B F  S 34 BBN 7 Li Q=1.6 MeV

13.   down to 93 keV 7 Be ≈ prompt g S 34 (0) = 0.567  0.018 keV barn