Carlo Broggini, INFN-Padova

Nuclear Burning in Stars

(Estar)

(E) = S(E) e–2E-1

2cm

mmmm

AstrophysicalFactor

GamowFactor

Reaction Rate(star) (E) (E) dE

Gamow Peak

MaxwellBoltzmann

Extrap. Meas.

NOW2004Laboratory measurements of

Astrophysical factors

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, R.Menegazzo, A.Ordine, 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)

LUNALUNA

m-2 h-1 n

cm-2 s-1

luna

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

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

measured2004-2005

3He (3He,2p)4He

Q = 12.86 MeV

min= 0.02 pb

Epmax= 10.7 MeV

from the Sun

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

S 14,1 /5

S 14,1 x5

Standard CF88

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

“High” energy: solid target + HpGe

14N(p,)15Og.s. transition

S gs(0)=0.25±0.06 keV b(LUNA)

S gs(0)=1.55±0.34 keV b (Schr87)

S tot(0)=1.7±0.1 ±0.2 keV b (LUNA) ~ 0.5

Globular cluster age: +0.7-1 Gy

cno ~ 0.5

S gs(0)=0.08+0.13–0.06 keV b

(Ang01)

Ebeam = 80 keV Low energy: gas target + BGO

(Estar) LUNA has shown that it is possible to measure

Past:

Present:

Future:

3He (3He,2p)4He from he Sun

14N(p,)15O cno

,Globular cluster age

3He(,)7Be the Sun

6.79 MeV transition

S 6.79(0)=1.63±0.17 keV b (Ang01)

S 6.79(0)=1.41±0.02 keV b (Schr87)

S 6.79(0)=1.35±0.05±0.08 keV b (LUNA)

14N(p,)15O

D abundance

Proto-stars

Big-bang

D(p,)3He

Q = 5.5. MeV

3He(,)7Be

Q=1.6 MeV

Solar Neutrinos Sun core properties

B

S1,7~

S(0)=0.53±0.05 keV b (Ad98)

S(0)=0.54±0.09 keV b (An99)

Solar thermometer

If S34/S34˜3-5% and B/B~3%

Better than Helioseismology

S3,40.84 * * T20

25Mg(p,)26Al

Q=6.3 MeV

Nucleosynthesis of 24<A<27

Astronomical interest of the from 26Al decay

(image taken by COMPTEL)