Laboratory measurements of
Astrophysical factors
Nuclear Burning
in Stars
Carlo Broggini, INFN-Padova
NOW2004
s(E)
s(Estar)
Gamow
Factor
Astrophysical
Factor
= S(E)
e–2ph
2ph = 31.29 Z1Z2 m/Ecm
m = m1m2 / (m1+m2)

Reaction Rate(star)  F(E) s(E) dE
Extrap.
Gamow Peak
Maxwell
Boltzmann
E-1
s
Meas.
LUNA
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, RuhrUniversität Bochum (GE)
•Centro de Fisica Nuclear da Universidade
de Lisboa (Portugal)
•Atomki Debrecen (Hungary)
Fm
= 0.7 m-2 h-1
F
-6 cm-2 s-1

310
n
luna
LUNA1 ( 50 kV)
Voltage Range :
1 - 50 kV
Output Current:
1 mA
Beam energy spread:
20 eV
Long term stability (8 h):
10-4
Terminal Voltage ripple:
5 10-5
LUNA2 (400 kV)
Voltage Range :50-400 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
pp chain
p + p  d + e+ + n e
d + p  3He + g
84.7 %
3He
+3He  a + 2p
3He
13.8 %
+4He  7Be + g
0.02 %
13.78 %
7Be+e- 7Li
7Li
measured
+ g +ne
+p  a + a
7Be
+ p  8B + g
8B
2a + e++ ne
2004-2005
3He (3He,2p)4He
Q = 12.86 MeV
Epmax= 10.7 MeV
n from the Sun
smin = 0.02 pb
14N(p,g)15O
Q=7.3 MeV
n E<1.2 MeV
n E<1.7 MeV
n F
cno

cno
S1,14
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)
S 14,1
/5
S 14,1 x5
Standard CF88
“High” energy: solid target + HpGe
gamma spectrum of
14N(p,g)15O
at Ep=140 keV
14N(p,g)15O
g.s. transition
S gs(0)=1.55±0.34 keV b
(Schr87)
S gs(0)=0.08+0.13–0.06 keV b
(Ang01)
S gs(0)=0.25±0.06 keV b
(LUNA)
S
tot(0)=1.7±0.1
n
cno
±0.2 keV b (LUNA)
~ 0.5
Globular cluster age:
+0.7-1 Gy
s
~ 0.5
Low energy: gas target + BGO
Ebeam = 80 keV
LUNA has shown that it is
possible to measure s(Estar)
Past:
3He
n from he Sun
(3He,2p)4He
Present:
14N(p,g)15O
Future:
3He(a,g)7Be
n
,Globular cluster age
cno
the Sun
14N(p,g)15O
6.79 MeV transition
S 6.79(0)=1.41±0.02 keV b
(Schr87)
S 6.79(0)=1.63±0.17 keV b
(Ang01)
S 6.79(0)=1.35±0.05±0.08
keV b (LUNA)
D(p,g)3He
Q = 5.5. MeV
D abundance
Proto-stars
Big-bang
3He(a,g)7Be
Q=1.6 MeV
Solar Neutrinos
F
B
Sun core properties
0.84
20
S
S
~ 1,7 * 3,4
T
*
Solar thermometer
S(0)=0.53±0.05 keV b (Ad98)
S(0)=0.54±0.09 keV b (An99)
If S34/S34˜3-5% and B/B~3%
Better than Helioseismology
25Mg(p,g)26Al
Q=6.3 MeV
Nucleosynthesis of 24<A<27
Astronomical interest of the g from 26Al decay
(image taken by COMPTEL)