Carlo Broggini, INFN-Padova Nuclear Burning in Stars (E star ) ( E ) = S(E) e –2 E -1 2 cm m m m m Astrophysical Factor Gamow Factor Reaction Rate(star)

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Presentation transcript:

Carlo Broggini, INFN-Padova Nuclear Burning in Stars (E star ) ( E ) = S(E) e –2 E -1 2 cm m m m m Astrophysical Factor Gamow Factor Reaction Rate(star) (E) (E) dE Gamow Peak Maxwell Boltzmann Extrap.Meas. NOW2004 Laboratory measurements of Astrophysical factors

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 INFN : Genova, LNGS, Milano, Napoli, Padova, Torino Inst.Physik mit Ionenstrahlen, Ruhr- Universität Bochum (GE) Centro de Fisica Nuclear da Universidade de Lisboa (Portugal) Atomki Debrecen (Hungary) LUNA

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

3 He ( 3 He,2p) 4 He Q = MeV min = 0.02 pb E p max = 10.7 MeV from the Sun

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

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

gamma spectrum of 14 N(p, ) 15 O at Ep=140 keV High energy: solid target + HpGe

14 N(p, g ) 15 O g.s. transition S gs (0)=0.25±0.06 keV b (LUNA) S gs (0)=1.55±0.34 keV b (Schr87) S tot (0)=1.7±0.1 ±0.2 keV b (LUNA) ~ 0.5 Globular cluster age: Gy cno ~ 0.5 S gs (0)= –0.06 keV b (Ang01)

Ebeam = 80 keV Low energy: gas target + BGO

(E star ) LUNA has shown that it is possible to measure Past: Present: Future: 3 He ( 3 He,2p) 4 He from he Sun 14 N(p, g ) 15 O cno,Globular cluster age 3 He(, g ) 7 Bethe Sun

6.79 MeV transition S 6.79 (0)=1.63±0.17 keV b (Ang01) S 6.79 (0)=1.41±0.02 keV b (Schr87) S 6.79 (0)=1.35±0.05±0.08 keV b (LUNA) 14 N(p, g ) 15 O

D abundance Proto-stars Big-bang D(p, g ) 3 He Q = 5.5. MeV

3 He(, g ) 7 Be Q=1.6 MeV Solar Neutrinos Sun core properties F B S 1,7 ~ S(0)=0.53±0.05 keV b (Ad98) S(0)=0.54±0.09 keV b (An99) Solar thermometer If S 34 /S 34 ˜ 3-5% and B / B ~3% Better than Helioseismology S 3, * * T 20

25 Mg(p, g ) 26 Al Q=6.3 MeV Nucleosynthesis of 24 < A < 27 Astronomical interest of the from 26 Al decay (image taken by COMPTEL)