Carlo Broggini, INFN-Padova Nuclear Burning in Stars  (E star )  ( E ) = S(E) e –2   E -1 2       m  m   m   m 

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Presentation transcript:

Carlo Broggini, INFN-Padova Nuclear Burning in Stars  (E star )  ( E ) = S(E) e –2   E -1 2       m  m   m   m   Reaction Rate(star)    (E)  (E) dE Gamow Peak  Maxwell Boltzmann Extrap.Meas.  LUNA and the Sun Men in pits or wells sometimes see the stars…. Aristotle

luna

LUNA2 ( 400 kV) Voltage Range : 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 LUNA1 ( 50 kV ) Voltage Range : kV Output Current: 1 mA Beam energy spread: 20 eV Long term stability (8 h): Terminal Voltage ripple:

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 % % 0.02% pp chain

3 He( , g ) 7 Be Solar Neutrinos: 7 Be, 8 B BBN 7 Li Q=1.6 MeV 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 %

  of 3 He( , g ) 7 Be down to 93 keV 7 Be ≈ prompt g S 34 (0) =  keV barn Δ Φ ( B ) reduced from 12% to 10% Δ Φ ( Be ) reduced from 9.4% to 5.5% (C. Pena Garay) Borexino-Kamland

14 N(p, g ) 15 O Q=7.3 MeV cno F  S 1,14 Globular Cluster Age S(0)= keV b (Ad98) S(0)= keV b (An99) E<1.2 MeV E<1.7 MeV

N+p 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

cno from the Sun Globular cluster age C yield in AGB stars S t (0)=1.61±0.18 keV b ‘clover’ study of the capture to the ground state: error on S t (0)= ±0.13 cno from the Sun solar core metallicity

2 H(α, g ) 6 Li Q=1.47 MeV 15 N(p, g ) 16 O Q=12.13 MeV (already started) 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 (almost completed) Rich program of Nuclear Astrophysics:

15 N(p, g ) 16 O

3 He( , g ) 7 Be: 14 N(p, g ) 15 O:  down to 70 keV (T=60 T 6 ) cno reduced by  2 with 8% error core metallicity Globular cluster age increased by 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 Δ Φ ( Be ) reduced from 9.4% to 5.5% 7 Be ≈ prompt g  down to 93 keV

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 Forschungszentrum Dresden-Rossendorf Atomki Debrecen LUNA