Carlo Broggini, INFNPadova

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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) e2ph E-1
2ph 31.29 Z1Z2 ?m/Ecm
m m1m2 / (m1m2)
?
Reaction Rate(star) ?
F(E) s(E) dE
Extrap.
Meas.
Gamow Peak
s
Maxwell Boltzmann
s
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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)
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F?
Fn

0.7 m-2 h-1
? 3?10-6 cm-2 s-1
luna
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LUNA2 (400 kV)
LUNA1 ( 50 kV)
Voltage Range 50-400 kV
Output Current 1 mA (_at_ 400 kV)


Absolute Energy error 300 eV Beam
energy spread lt100 eV Long term stability (1 h)
5 eV Terminal Voltage ripple 5 Vpp Ge detector
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
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3He (3He,2p)4He
Q 12.86 MeV
Epmax 10.7 MeV
? from the Sun
?min
0.02 pb
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14N(p,g)15O
Q7.3 MeV
? Elt1.2 MeV
? Elt1.7 MeV

• ?

F
S1,14
?
cno
cno

• Globular Cluster Age

S(0)3.5-1.60.4 keV b (Ad98)
S(0)3.2-0.80.8 keV b (An99)
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• High energy solid target HpGe

gamma spectrum of 14N(p,g)15O at Ep140 keV
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14N(p,g)15O
g.s. transition
S gs(0)1.550.34 keV b (Schr87)
S gs(0)0.080.130.06 keV b (Ang01)
S gs(0)0.250.06 keV b (LUNA)
s
S tot(0)1.70.1 0.2 keV b (LUNA)
0.5
?cno 0.5
PLB 591(2004)61 AA 420(2004)625
Globular cluster age 0.7-1 Gy
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Calorimeter
10-7 mbar
10-6 mbar
10-4 mbar
BGO
0.5-2 mbar
Windowless gas-target Max 10 mbar
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• Low energy gas target BGO

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• LUNA has shown that it is

s(Estar)
possible to measure
? from he Sun

3He (3He,2p)4He

14N(p,g)15O
Novae AGB stars RGB stars Globular cluster
?
cno