Download - Carlo Broggini, INFN-Padova Nuclear Burning in Stars (E star ) ( E ) = S(E) e –2 E -1 2 m m m m
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Carlo Broggini, INFN-Padova
Nuclear Burning in Stars
(Estar)(E) = S(E) e–2E-1
2
mmmmReaction Rate(star) (E) (E) dE
Gamow Peak
MaxwellBoltzmann
Extrap. Meas.
LUNA and the Sun
Men in pits or wells sometimes
see the stars…. Aristotle
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luna
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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
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
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p + p d + e+ + e
d + p 3He +
3He +3He +2p 3He +4He 7Be +
7Be+e- 7Li + +e 7Be + p 8B +
7Li + p 8B 2 + e++ e
84.7 % 13.8 %
13.78 % 0.02%
pp chain
0,45
0,47
0,49
0,51
0,53
0,55
0,57
80 100 120 140 160 180
Ecm [keV]
S(E
) [k
eV b
]
activation-PRL+PRC
activation
on-line
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3He(,)7Be
Solar Neutrinos:7Be,8BBBN 7Li
Q=1.6 MeV
•Cross section from prompt gammaprompt gamma down to 90 keV (CM energy) using 4He beam on 3He target•Activation via off-line radioactive decayradioactive decay measurements of the 7Be atoms collected in the beam catcher•All with a final error < 5 %
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of 3He(,)7Be down to 93 keV 7Be ≈ prompt
SS3434(0) = 0.560 (0) = 0.560 0.017 keV barn 0.017 keV barn
ΔΦ(B) reduced from 12% to 10%
ΔΦ(Be) reduced from 9.4% to 5.5% (C. Pena Garay)
Borexino-Kamland
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14N(p,)15O
Q=7.3 MeV
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)
E<1.2 MeV
E<1.7 MeV
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- 504
-21
278
1414N+pN+p
729772977556
7276
68596793
6176
5241
5183
01515OO
1/2 +
7/2 +
5/2 +
3/2 +
3/2 -
5/2 +
1/2 +
1/2 -
“High” energy: solid target + HpGe
gamma spectrum of 14N(p,)15O at 140 keV beam energy
14N(p,)15OLow energy: gas target + BGO
beam energy 90 keV
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cno from the Sun Globular cluster age C yield in AGB stars
St(0)=1.61±0.18 keV b‘clover’ study of the capture to the ground state: error on St(0)= ±0.13
cno from the Sun solar core metallicity
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2H(α,)6Li Q=1.47 MeV
15N(p,)16O Q=12.13 MeV(already started)
17O(p,)18F Q=5.6 MeV
23Na(p,)24Mg Q=11.7 MeV
22Ne(p,)23Na Q=8.8 MeV
18O(p,)19F Q=8.0 MeV
25Mg(p,)26Al Q=6.3 MeV(almost completed)
Rich program of Nuclear Astrophysics:
............
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15N(p,)16O
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3He(,)7Be:
14N(p,)15O: down to 70 keV (T=60 T6)
cno reduced by 2 with 8% error core metallicity Globular cluster age increased by 0.7-1 Gy Higher C yield in AGB stars
LUNA has shown that it is possible to measure
(Estar): 3He (3He,2p)4He, 2H(p,)3He 3He (3He,2p)4He: down to 16 keV
no resonance within the solar Gamow Peak
ΔΦ(Be) reduced from 9.4% to 5.5%
7Be ≈ prompt
down to 93 keV
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INFN - Laboratori Nazionali del Gran Sasso
D.Bemmerer,R.Bonetti,C.Broggini,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
LUNALUNA