1.  s 2ph = 31.29 Z1Z2 m/E m = m1m2 / (m1+m2), E in keV
Astrofisica nucleare al Gran Sasso
Carlo Broggini
INFN-Padova
Men in pits or wells sometimes see the stars….
Aristotle
Stellar Energy+Nucleosynthesis
Hydrogen Burning
s(Estar) with Estar << ECoulomb
s(E) = S(E) e–2ph E-1
2ph = Z1Z2 m/E
m = m1m2 / (m1+m2), E in keV 
Reaction Rate(star) 
F(E) s(E) dE s
Gamow Peak
Extrap.
Meas.
S(E)
Maxwell
Boltzmann

2. Background due to cosmic rays:
* Electromagnetic component (removed by ~10 cm of lead)
* Hadrons (removed by a few meters of concrete)
* Low energy negative muons : capture and production of radioactive nuclei (1-10 s lifetime, delayed gamma ray emission )
* High energy muons: ionization + spallation giving rise to radioactive nuclei (1-10 s lifetime, delayed gamma ray emission ) and neutrons . Because of the delayed gamma rays active veto are not very effective and passive shields to suppress natural radioactivity have to be ‘light’ (10-15 cm of lead)
Muon suppression:
Vertical muon intensity above 1 GeV/c at sea level:
~70 m-2s-1sr-1, angular distribution ÷ cos2θzenith
To suppres muons a shield of at least 1 km of water equivalent is required (1 km w.e. = 105 gr/cm2 ~ 300 meters of rock).
The flat region at large depths is due to neutrino-induced
muons of energy above 2 GeV

3. 1400 m of dolomite rock, CaMg(CO3)2, (~3800 m w.e.)
1979 Gran Sasso Lab proposed by A. Zichichi
1989 first underground experiment ON
1400 m of dolomite rock, CaMg(CO3)2, (~3800 m w.e.)
Surf.: m2, Vol.: m3, Ventilation: 1 vol / 3.5 hours (Rn in air Bq m-3)
Muon flux: 1.1 m-2h-1, 6 orders of magnitude reduction
Neutron flux, mainly from (,n) : cm-2s-1 (0-1 keV), cm-2s-1 (> 1 keV), 3 orders of magnitude reduction
Gamma rays: only 1 order of magnitude reduction, but with thick shield (no muon activation) about 5 orders of magnitude in the region of natural radioactivity and 4-5 orders above 3.2 MeV without any shield (gamma rays due to n-interaction)

4. Laboratory for Underground Nuclear Astrophysics: LUNA
50 kV
400 kV
3.5 MV
Beam: H,He
Voltage Range : kV
Output Current: ~1 mA
Absolute Energy error
±300 eV
Beam energy spread:
<100 eV
Long term stability (1 h) :
5 eV
Terminal Voltage ripple:
5 Vpp Ge detector

5. e Hydrogen burning in the Sun @15*106 degrees: 6*1011 kg/s H He
+0.7% MH E e
4H He +2e+ + 2
MeV
3He burning in the p-p chain
No ghost solar Gamow peak
Activation=prompt gamma
no monopole contribution to s
s at low energy with 4% error

6. 3He (3He,2p)4He
Q = MeV
Epmax= 10.7 MeV
Suppression of 7Be and 8B e due to a resonance in 3He (3He,2p)4He
which modifies the neutrino spectrum?
H+, 3He+ beam
Voltage Range: kV
Output Current: 1 mA
Beam energy spread: 20 eV
Long term stability (8 h): 10-4
Terminal Voltage ripple:
Windowless gas target 0.5 mbar) + 8 silicon detectors (5cmx5cm, 1mmthick)

7. smin=20 fb (2 events/month)
No resonance at the Gamow peak
Nuclear astrophysics is not the reason for the
suppression of e from the Sun

8. *½cno from the Sun * Globular Cluster age +1Gy
The CNO Cycle
278
7556
1/2 +
1) “High” energy: solid target + HpGe
7297
7276
7/2 +
2) Low energy: gas target + BGO
14N+p
14N(p,g)15O
6859
5/2 +
-21
beam energy 90 keV
13C
(p,g)
14N
15O b+
(p,a)
12C
13N
15N
6793
3/2 +
- 504
6176
3/2 -
5241
5/2 +
5183
1/2 +
(p,g)
15O
1/2 -
16O
St(0)=1.57±0.13 keV b
as reported by indirect measurements
(Mukhamedzhanov et al. 2003)
*½cno from the Sun
* Globular Cluster age +1Gy
* more C at the surface of AGB
cno = F(S1,14,Zcore)
probe of the metallicity Z of the Sun core

9. AGB stars (~30-100 T6), Nova nucleosynthesis (~100-400 T6) and BBN
LUNA beyond the Sun: isotope production in the hydrogen burning shell of
AGB stars (~ T6), Nova nucleosynthesis (~ T6) and BBN
Nova Cigni 1992

10. 2H(α,g)6Li Q=1.47 MeV 22Ne(p,g)23Na Q=8.8 MeV 15N(p,g)16O Q=12.13 MeV
Isotopic abundances: how and where
15N(p,g)16O Q=12.13 MeV
25Mg(p,g)26Al Q=6.3 MeV
17O(p,g)18F Q=5.6 MeV
2H(α,g)6Li Q=1.47 MeV
17O(p,α)14N Q=1.2 MeV
22Ne(p,g)23Na Q=8.8 MeV
18O(p,α)15N Q=4.0 MeV
23Na(p,g)24Mg Q=11.7 MeV
18O(p,g)19F Q=8.0 MeV

11. ● Uncertainty on 16O, 17O and 19F at Nova temperature less than 10%
● First measurement of the 92 keV resonance in 25Mg(p, g)26Al, ωγ=(2.9±0.6)x 10-10eV. Production of 26Algs in H-burning regions is less efficientthan previously obtained (Sky 1.8 MeV)
● Uncertainty on 16O, 17O and 19F at Nova temperature less than 10%
(from 40-50%)
● First measurement of D(α, g)6Li at the BBN energies:
6Li/7Li =(1.5±0.3)*10-5, no nuclear solution to the primordial 6Li problem

12. The Ne-Na Cycle 22Ne(p,g)23Na
Only upper limits (~μeV) on the strength of the resonances below 400 keV (factor 1000 on the reaction rate)
Ne, Na, Mg and Al yield in AGB
and Novae (up to a factor 100)
22Ne(p,g)23Na
Q=8.8 MeV
103

13. ● 2 HPGe detectors collimated at 55° (130%) and 90° (88%)
● Windowless gas target with recirculation 22Ne enriched at 99.9%, effective target length: 8 cm ~ 4 keV
● 2 HPGe detectors collimated at 55° (130%) and 90° (88%)
● Cu+Pb (~ 30 cm) + anti-Radon shielding
● Resonances studied with a few neV strength sensitivity
and 700 eV uncertainty on the energy
● 156.2, and keV resonances measured for the first time
● New upper limits on 71, 105 and 215 keV
● Yield measured at 291, 320 and 334 keV compatible with Direct Capture
R. Depalo NPA VII York, 18 – 22 May 2015
12/25

14. PRELIMINARY
Now: Windowless gas target + BGO high efficiency detector to study the low
energy region. 71 and 105 keV (~0.01 neV strength sensitivity) + Direct Capture (D. Piatti talk tomorrow)

15. cno reduced by  2 with 8% error Sun core metallicity
3He (3He,2p)4He: s down to 16 keV
no resonance within the solar Gamow Peak
3He(,g)7Be:
7Be ≈ prompt g
cross section measured with 4% error
14N(p,g)15O: s down to 70 keV
cno reduced by  2 with 8% error Sun core metallicity
Globular cluster age increased by Gy
More carbon at the surface of AGB stars
25Mg(p,g)26Al: first measurement of the 92 keV resonance,
strength ωγ=(2.9±0.6)x eV
Uncertainty on 16O, 17O and 19F from Novae less than 10% (from 40-50%)
22Ne(p,g)23Na: 3 resonances in the Nova region measured for the first time, high efficiency measurement running

16. The LUNA collaboration
A. Best, A. Boeltzig*, A. Formicola, S. Gazzana, I. Kochanek, M. Junker, L. Leonzi | INFN LNGS /*GSSI, Italy
D. Bemmerer, M. Takacs, T. Szucs | HZDR Dresden, Germany
C. Broggini, A. Caciolli, R. Depalo, R. Menegazzo, D. Piatti | Università di Padova and INFN Padova, Italy
C. Gustavino | INFN Roma1, Italy
Z. Elekes, Zs. Fülöp, Gy. Gyurky| MTA-ATOMKI Debrecen, Hungary
O. Straniero | INAF Osservatorio Astronomico di Collurania, Teramo, Italy
F. Cavanna, P. Corvisiero, F. Ferraro, P. Prati, S. Zavatarelli | Università di Genova and INFN Genova, Italy
A. Guglielmetti, D. Trezzi | Università di Milano and INFN Milano, Italy
A. Di Leva, G. Imbriani, | Università di Napoli and INFN Napoli, Italy
G. Gervino | Università di Torino and INFN Torino, Italy
M. Aliotta, C. Bruno, T. Davinson | University of Edinburgh, United Kingdom
G.F. Ciani, G. D’Erasmo, E.M. Fiore, V. Mossa, F. Pantaleo, V. Paticchio, R. Perrino, L. Schiavulli, A. Valentini| Università di Bari and INFN Bari, Italy