1 / 16

Carlo Broggini, INFN-Padova

Laboratory measurements of Astrophysical factors. Carlo Broggini, INFN-Padova. NOW2004. Gamow Factor. Astrophysical Factor. Nuclear Burning in Stars s (E star ). s ( E ) = S(E) e –2 ph E -1. 2 ph = 31.29 Z 1 Z 2 m/E cm. m = m 1 m 2 / ( m 1 + m 2 ). .

elvis-mccormick
Télécharger la présentation

Carlo Broggini, INFN-Padova

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Laboratory measurementsof Astrophysical factors Carlo Broggini, INFN-Padova NOW2004 Gamow Factor Astrophysical Factor • Nuclear Burning • in Stars • s(Estar) s(E) = S(E) e–2phE-1 2ph = 31.29 Z1Z2m/Ecm m = m1m2 / (m1+m2)  Reaction Rate(star)  F(E) s(E) dE Extrap. Meas. Gamow Peak s Maxwell Boltzmann s

  2. LUNA 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)

  3. F Fn = 0.7m-2 h-1 310-6cm-2 s-1 luna

  4. LUNA1 ( 50kV) LUNA2 (400kV) 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 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

  5. p + p  d + e+ + ne d + p  3He + g pp chain 84.7 % 13.8 % 3He +3He  a + 2p 3He +4He  7Be + g 0.02 % 13.78 % 7Be +p  8B + g 7Be+e- 7Li + g +ne 7Li +p  a + a 8B 2a + e++ ne 2004-2005 measured

  6. 3He (3He,2p)4He Q = 12.86 MeV Epmax= 10.7 MeV  from the Sun min = 0.02 pb

  7. 14N(p,g)15O Q=7.3 MeV E<1.2 MeV E<1.7 MeV •  F S1,14  cno cno • 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)

  8. S 14,1 /5 S 14,1 x5 Standard CF88

  9. “High” energy: solid target + HpGe gamma spectrum of 14N(p,g)15O at Ep=140 keV

  10. 14N(p,g)15O g.s. transition S gs(0)=1.55±0.34 keV b (Schr87) S gs(0)=0.08+0.13–0.06 keV b (Ang01) S gs(0)=0.25±0.06 keV b (LUNA) s S tot(0)=1.7±0.1 ±0.2 keV b (LUNA) ~ 0.5 cno ~ 0.5 Globular cluster age: +0.7-1 Gy

  11. Low energy: gas target + BGO Ebeam = 80 keV

  12. LUNA has shown that it is s(Estar) possible to measure  from he Sun • Past: 3He (3He,2p)4He  • Present: 14N(p,g)15O ,Globular cluster age cno • Future: 3He(,g)7Be the Sun

  13. 14N(p,g)15O 6.79 MeV transition S 6.79(0)=1.41±0.02 keV b (Schr87) S 6.79(0)=1.63±0.17 keV b (Ang01) S 6.79(0)=1.35±0.05±0.08 keV b (LUNA)

  14. D(p,g)3He Q = 5.5. MeV • D abundance • Proto-stars • Big-bang

  15. 3He(,g)7Be Q=1.6 MeV • Solar Neutrinos Sun core properties F S1,7 S3,40.84 ~ T20 * * B Solar thermometer S(0)=0.53±0.05 keV b (Ad98) S(0)=0.54±0.09 keV b (An99) If S34/S34˜3-5% and B/B~3% Better than Helioseismology

  16. 25Mg(p,g)26Al Q=6.3 MeV • Nucleosynthesis of 24<A<27 the  from 26Al decay • Astronomical interest of (image taken by COMPTEL)

More Related