1.  s(E) = S(E) e–2ph E-1 s Nuclear Burning in Stars s(Estar) s
LUNA and the neutrinos
from the Sun
Carlo Broggini,
INFN-Padova
Men in pits or wells sometimes see the stars…. Aristotle
Nuclear Burning
in Stars
s(Estar)
s(E) = S(E) e–2ph E-1
2ph = Z1Z2 m/E 
Reaction Rate(star) 
F(E) s(E) dE
m = m1m2 / (m1+m2)
Gamow Peak
Extrap.
Meas. s
Maxwell
Boltzmann s

2. Laboratory for Underground
Nuclear Astrophysics

3. 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

4. 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

5. F  S34 3He(,g)7Be Solar Neutrinos: 7Be,8B BBN 7Li Q=1.6 MeV
Cross section from prompt gamma using 4He beam on 3He target
from off-line radioactive decay of the 7Be atoms collected in the beam catcher
All with a final error < 5 %

6. s down to 93 keV S34(0) = 0.560  0.017 keV barn 7Be ≈ prompt g
ΔΦ(B) reduced from 12% to 10% (C. Pena-Garay)
ΔΦ(Be) reduced from 9.4% to 5.5%
Borexino-Kamland

7. F  Globular Cluster Age S1,14 14N(p,g)15O cno cno  Q=7.3 MeV 278
7556
1/2 +
14N(p,g)15O
7297
7276
7/2 +
14N+p
6859
5/2 +
-21
6793
Q=7.3 MeV
3/2 +
- 504
6176
3/2 -  F
S1,14
5241
5/2 +
cno 
cno
5183
1/2 +
Globular Cluster Age
15O
1/2 -

8. solar core metallicity homogeneous zero-age Sun
St(0)=1.61±0.18 keV b
* ½cno from the Sun
* Globular cluster age
* C yield in AGB stars
New study with a ‘clover’
detector of the capture
to the ground state
St(0)=1.57±0.13 keV b (to be published in PRC)
From a measurement of cno from the Sun
solar core metallicity
homogeneous zero-age Sun

9. ............ Rich program of Nuclear Astrophysics:
25Mg(p,g)26Al Q=6.3 MeV
(almost completed)
2H(α,g)6Li Q=1.47 MeV
17O(p,g)18F Q=5.6 MeV
18O(p,g)19F Q=8.0 MeV
22Ne(p,g)23Na Q=8.8 MeV
23Na(p,g)24Mg Q=11.7 MeV
15N(p,g)16O Q=12.13 MeV
(already started)

10. 3He (3He,2p)4He: s down to 16 keV
no resonance within the solar Gamow Peak
3He(,g)7Be:
7Be ≈ prompt g
ΔΦ(Be) reduced from 9.4% to 5.5%
14N(p,g)15O: s down to 70 keV (T=60 T6)
cno reduced by  2 with 8% error core metallicity
Globular cluster age increased by Gy
Higher C yield in AGB stars

11. New underground accelerators:
Gran Sasso, DUSEL, Boulby mine, Canfranc, Romania…
12C(a,g)16O
13C(a,n)16O
22Ne(a,n)25Mg
(a,g) on 14N, 15N, 18O……

12. LUNA INFN - Laboratori Nazionali del Gran Sasso
D.Bemmerer,R.Bonetti,C.Broggini, A.Caciolli,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