Underground Nuclear Astrophysics and Solar Neutrinosfusion06/talks/Wednesday/broggini.pdf ·...

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Nuclear Burning in Stars σ (E star ) s(E) = S(E) e –2ph E -1 Reaction Rate(star) F (E) s (E) dE Gamow Peak Maxwell Boltzmann Extrap. Meas. s Underground Nuclear Astrophysics and Solar Neutrinos Men in pits or wells sometimes see the stars…. Aristotle Carlo Broggini, INFN-Pd

Transcript of Underground Nuclear Astrophysics and Solar Neutrinosfusion06/talks/Wednesday/broggini.pdf ·...

Page 1: Underground Nuclear Astrophysics and Solar Neutrinosfusion06/talks/Wednesday/broggini.pdf · Underground Nuclear Astrophysics and Solar Neutrinos ... Aristotle Carlo Broggini, INFN-Pd.

Nuclear Burning in Starsσ(Estar) σ(E) = S(E) e–2πη E-1

Reaction Rate(star) ÷∫Φ(E) σ(E) dE

Gamow Peak

MaxwellBoltzmann

Extrap. Meas.

σ

Underground Nuclear Astrophysics and Solar NeutrinosMen in pits or wells sometimes

see the stars…. Aristotle

Carlo Broggini, INFN-Pd

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INFN - Laboratori Nazionalidel Gran SassoD.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 (GE)

•Atomki Debrecen (Hungary)

LUNALUNA

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Φµ= 0.7 m-2 h-1 Φn ≈ 3∗10−6 cm-2 s-1

luna

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LUNA2 (400 kV)

Voltage Range :50-400 kVOutput 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+ + νe

d + p → 3He + γ

3He +3He → α + 2p 3He +4He → 7Be + γ

7Be+e-→ 7Li + γ +νe7Be + p → 8B + γ

7Li + p → α + α 8B→ 2α + e++ νe

84.7 % 13.8 %

13.78 % 0.02 %

pp chain

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3He (3He,2p)4He

Q = 12.86 MeV

σmin = 0.02 pb

Epmax= 10.7 MeV

ν from the Sun

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14N(p,γ)15OQ=7.3 MeV

νcno Φcno∼ S1,14

Globular Cluster Age

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gamma spectrum of 14N(p,γ)15O at Ep=140 keV

“High” energy: solid target + HpGe

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10-7 mbar 10-6 mbar 10-4 mbar

0.5-2 mbar

Windowless gas-targetMax 10 mbar

Low energy: gas target + BGO

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beam energy: 90 keV

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3He(α,γ)7BeQ=1.6 MeV

Solar Neutrinos Sun core properties(largest nuclear physics uncertainty in the SSM)

Big-Bang 7Li

• Cross section of direct decaydirect decay down to 60-70 keV (CM energy) using 4He beam on 3He target

• Reaction Yield around 100-150 keV (CM energy) via off-line radioactive decayradioactive decay measurements of the recoils collected in the beam catcher

• All with a final error < 5 %

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HPGe

Lead shield

1st2nd3rd

Expected attenuation for1.6 MeV γs: 10-5-10-6

(GEANT4 simulations)

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Movable silicon detector for I*ρ measurement

Removable calorimeter cap for off-line 7Be-activity measurement

33He gasHe gas

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3He(α,γ)7Be the Sun, big-bang 7Li

14N(p,γ)15O: σ down to 70 keV (T=60 T6)

νcno from the Sun reduced by ∼ 2Globular cluster age increased by 0.7-1 GyHigher C yield in AGB stars

LUNA has shown that it is possible to measureσ(Estar): 3He (3He,2p)4He, 2H(p,γ)3He

3He (3He,2p)4He: σ down to 16.5 keVno resonance within the solar Gamow Peak

Page 19: Underground Nuclear Astrophysics and Solar Neutrinosfusion06/talks/Wednesday/broggini.pdf · Underground Nuclear Astrophysics and Solar Neutrinos ... Aristotle Carlo Broggini, INFN-Pd.

D abundance

Proto-stars

Big-bang

D(p,γ)3HeQ = 5.5. MeV

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S 14,1 /5

S 14,1 x5

Standard CF88

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25Mg(p,γ)26AlQ=6.3 MeV

Nucleosynthesis Mg-Al

Astronomical interest of the γ from 26Al decay

•Cross section at 180-400 keV (CM energy) using GeGedetectorsdetectors (not underground)

•Cross section at lower energies using BGO summing BGO summing crystalscrystals (underground)