1.  s(E) = S(E) e–2ph E-1 s Laboratory for Underground
Nuclear Astrophysics
Carlo Broggini, INFN-Padova
NUPECC-Venezia
Gamow
Factor
Astrophysical
Factor
Nuclear Burning
in Stars
s(Estar)
s(E) = S(E) e–2ph E-1
2ph = Z1Z2 m/Ecm
m = m1m2 / (m1+m2) 
Reaction Rate(star) 
F(E) s(E) dE
Extrap.
Meas.
Gamow Peak s
Maxwell
Boltzmann s

2. LUNA Men in pits or wells sometimes see the stars…. Aristotle
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, B.Limata, R.Menegazzo, 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)

4. F Fn
= 0.7 m-2 h-1
 310-6 cm-2 s-1
luna

5. LUNA1 ( 50 kV) LUNA2 (400 kV) Voltage Range :50-400 kV Voltage Range :
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
Voltage Range : kV
Output Current:
1 mA
Beam energy spread:
20 eV
Long term stability (8 h):
10-4
Terminal Voltage ripple:
5 10-5

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

7.  from the Sun min 3He (3He,2p)4He Q = 12.86 MeV Epmax= 10.7 MeV
= 0.02 pb

8. F  E<1.2 MeV  E<1.7 MeV  Globular Cluster Age S1,14
14N(p,g)15O
Q=7.3 MeV
 E<1.2 MeV
 E<1.7 MeV  F 
S1,14
cno
cno
Globular Cluster Age
S(0)= keV b (Ad98)
S(0)= keV b (An99)

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

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

12. cno ~ 0.5 s 14N(p,g)15O ~ 0.5 S tot(0)=1.7±0.1 ±0.2 keV b (LUNA)
g.s. transition
S gs(0)=1.55±0.34 keV b
(Schr87)
S gs(0)= –0.06 keV b
(Ang01)
S gs(0)=0.25±0.06 keV b
(LUNA) s
S tot(0)=1.7±0.1 ±0.2 keV b (LUNA)
~ 0.5
cno ~ 0.5
PLB 591(2004)61
A&A 420(2004)625
Globular cluster age: Gy

13. Windowless gas-target
Calorimeter
10-7 mbar
10-6 mbar
10-4 mbar
BGO
0.5-2 mbar
Windowless gas-target
Max 10 mbar

14. Low energy: gas target + BGO

16.  from he Sun  s(Estar) LUNA has shown that it is cno
possible to measure
 from he Sun
3He (3He,2p)4He
14N(p,g)15O
Novae
AGB stars
RGB stars
Globular cluster 
cno