1. Why going underground g-background
Gran Sasso shielding: 3800 m w.e.
40K
E>3.5MeV
Counts/keV/hours
0.33
214Bi
232Th
cosmic rays
Environmental radioactivity
Therefore, the advantage of an underground environment is evident for high Q-value reactions such as 14N(p,)15O, 15N(p,)16O, 17O(p,)18F, 25Mg(p,)26Al......
Radiation
LNGS/out
muons
neutrons
10-6
10-3

2. Why going underground n-background
Therefore, the advantage of an underground environment is evident for n-source reaction as 13C(a,n)16O, 22Ne(a,n)25Mg
Radiation
LNGS/out
muons
neutrons
10-6
10-3

3. Underground Pb-shielding and Radon box
HPGe fully sorrounded (55°) with 15 cm of Pb

4. 25Mg(p,)26Al - HPGe spectra ER = 190 keV

5. LUNA –> 1991-2017 LNGS Lab LUNA I 50 kV LUNA II 400 kV
Voltage Range : kV
Output Current:
1 mA
Beam energy spread:
20 eV
LNGS Lab
LUNA I
50 kV
Voltage Range : kV
Output Current:
500 mA
Beam energy spread:
70 eV
LUNA II
400 kV

6. p(d,g)3He, d(a,g)6Li, 3He(3He, 2p)4He, 3He(a,g)7Be14N(p,g)15O
LUNA ->
BBN and H-burning in the Sun and solar neutrinos:
p(d,g)3He, d(a,g)6Li, 3He(3He, 2p)4He, 3He(a,g)7Be14N(p,g)15O
Age of Globular Clusters and C production in AGB:
14N(p,g)15O
AGB nucleosynthesis – light nuclei abundances:
14N(p,g)15O, 15N(p,g)16O, 17O(p,g)18F, 17O(p,a)14N, 18O(p,g)19F, 18O(p,a)15N, 22Ne(p,g)23Na, 23Na(p,g)24Mg, 25Mg(p,g)26Al

7. LUNA MV – future setup
LNGS Lab
LUNA-MV 2019
3.5 MV

8. Layout of the new LUNA-MV facility
Thanks to MIUR by 2 «progetti premiale»
total grant: 5.3 M€
5.5 m
27 m
12.5 m
NPA VIII, LNS-Catania

9. The accelerator and the neutron shielding
1H+ (TV: 0.3 – 0.5 MV): μA
inline Cockcroft Walton accelerator
TERMINAL VOLTAGE: 0.2 – 3.5 MV
Precision of terminal voltage reading: 350 V
Beam energy reproducibility: 0.01% TV
Beam energy stability: 0.001% TV / h
Beam current stability: < 5% / h
1H+ (TV: 0.5 – 3.5 MV): 1000 μA
4He+ (TV: 0.3 – 0.5 MV): 300 μA He
4He+ (TV: 0.5 – 3.5 MV): 500 μA
12C+ (TV: 0.3 – 0.5 MV): 100 μA C
12C+ (TV: 0.5 – 3.5 MV): 150 μA
12C++ (TV: 0.5 – 3.5 MV): 100 μA
80 cm thick concrete shielding calculated by GEANT4 & MCNP
En = 5.6 MeV, n/s, isotropic
DA COMPATTARE CON LA PRECEDENTE
MCNP: Fn = n/(cm2 s)
GEANT4: Fn = n/(cm2 s)
Fn(LNGS) = n/(cm2 s)
NPA VIII, LNS-Catania

10. LUNA future measurements
Main neutron sources:
13C(a,n)16O, 22Ne(a,n)25Mg
Explovive CNO burning:
15O(a,g)19Ne, 14O(a,g)18Ne, 18Ne(a,p)21Na
He and advaced burnings:
12C(a,g)16O, 12C(12C, p)23Na, 12C(12C,a)20Ne, 16O(a,g)20Ne

11. LUNA-MV basic schedule
Action
Date
Approval of the first HVEE technical design
October 2016
Opening of the tendering procedure for LUNA-MV plants
November 2016
Submission of the Authorization request to «Prefettura dell’Aquila»
December 2016
Beginning of the clearing works in Hall B
February 2017
End of the tendering procedure for the new LUNA-MV building
June 2017
Beginning of the construction works in Hall B
September 2017
End of the tendering procedure for LUNA-MV plants
October 2017
Beginning of the construction of the plants in the LUNA-MV building
December 2017
Completion of the new LUNA-MV building and plants
April 2018
In-house acceptance test for the new LUNA-MV accelerator
May 2018
LUNA-MV accelerator delivering at LNGS
July 2018
Conclusion of the commissioning phase
December 2018
Beginning First Experiment
January 2019

12. LUNA MV- scientific program (2018  2022)
Commissioning measurement: 14N(p,g)15O.
High scientific interest for revised data covering a wide energy range (400 keV- 3.5 MeV). Scientific results of high impact but reduced risk immediately after commissioning phase
12C+12C: solid state target. Gamma and particle detectors
13C(a,n)16O: enriched 13C solid or gas target. Neutron detector
22Ne(a,n)25Mg: enriched 22Ne gas target. Neutron detector.
Next steps (not before 2023…):
12C(a,g)16O: 12C solid target depleted in 13C and alpha beam or a jet gas target and 12C beam.

13. Stellar environments for s-process
WEAK : Massive stars 22Ne(a,n)25Mg T> 109 K nn= cm-3 MAIN : low mass AGB (1-3 M⊙) 13C(a,n)16O (dominant) T=  106 K nn= cm-3 22Ne(a,n)25Mg (marginal) T=  106 K nn= cm-3

14. Experimental Results – 13C(a,n)16O

15. Experimental Results – 13C(a,n)16O
some conclusion:
- low energy data points do not constrain the fit with respect to the subthreshold resonance - quoted uncertainties are large  probably also a mixture of systematic and statistical uncertainties, e.g. in Drotleff scattering of data is unexpectely small with respect to error bars - most data point below E = 350 keV are higher than the fit curves, i.e. Heil R-matrix curve  indication for beam induced background?

16. Carbon burning in stars

17. 12C+12C - Total S-factor

18. Carbon burning in stars

19. Experimental results in g-ray spectrometry
Underground laboratory is the best place to get lower energy

20. Underground Pb-shielding and Radon box
HPGe fully sorrounded (55°) with 15 cm of Pb

21. Long-Term Developments
LUNA-MV
JUNA/CJPL
CASPAR
New underground facilities will open up exiting new opportunities for further major breakthrough in the field

22. The LUNA COLLABORATION (as of May 2017)
G.F. Ciani*, L. Csedreki, L. Di Paolo, A. Formicola, I. Kochanek, M. Junker, - INFN LNGS /*GSSI, Italy
D. Bemmerer, K. Stoeckel, M. Takacs, - 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, T. Szucs -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, -Università di Milano and INFN Milano, Italy
A. Best, 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. Chillery, T. Davinson - University of Edinburgh, United Kingdom
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
NPA VIII, LNS-Catania