Nuclear astrophysics of the s- and r-process
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1 Nuclear astrophysics of the s- and r-process René Reifarth Goethe University Frankfurt Ecole Joliot Curie School on Neutrons and Nuclei Frejus, France, Sep-28 Oct
2 Nucleosynthesis tales from the past Oct 2-3, 2014 René Reifarth 2
3 The nucleosynthesis of the elements intermediate neutron capture (i-process) Oct 2-3, 2014 René Reifarth 3
4 Radioctive isotopes in the s-process Oct 2-3, 2014 René Reifarth 4
5 Radioctive isotopes in the s-process Oct 2-3, 2014 René Reifarth 5
6 Radioctive isotopes in the s-process Oct 2-3, 2014 René Reifarth 6
7 Meteorites hints from the sky Meteorites contain presolar grains! Oct 2-3, 2014 René Reifarth 7
8 proton number the s-process Zr 80 Br, t 1/2 =17 min, 92 % (b - ), 8 % (b + ) Y Sr (n,g) Rb (b - ) (b + ) Ge Ga Zn Cu Ni Co Fe p-only Kr Br s-only Se As 85 Kr, t 1/2 =11 a 79 Se, t 1/2 =65 ka r-only 64 Cu, t 1/2 =12 h, 40 % (b - ), 60 % (b + ) 63 Ni, neutron t 1/2 =100 number a Oct 2-3, 2014 René Reifarth 8
9 MASS COORDINATE (M ) s-process in AGB stars Nucleosynthesis 0.68 convective envelope H - burning He - burning 0.67 He intershell 13 C(a,n) 22 Ne(a,n) 0.66 C-O - core TIME (a) Oct 2-3, 2014 René Reifarth 9
10 s-process nucleosynthesis Two components were identified and connected to stellar sites: Main s-process 90<A<210 Weak s-process A<90 TP-AGB stars 1-3 M shell H-burning He-flash K K kt=8 kev kt=25 kev cm cm C(a,n) 22 Ne(a,n) massive stars > 8 M core He-burning shell C-burning K ~ K kt=25 kev kt=90 kev 10 6 cm cm Ne(a,n)
11 s-process models - classical s-process 85 Kr (10 yr) n b Oct 2-3, 2014 René Reifarth 11
12 s-process models T-AGB stars, 22 Ne phase 95 Zr (64 d) n b Couture & Reifarth, ADNDT, 93 (2007) 807 Oct 2-3, 2014 René Reifarth 12
13 r-process Oct 2-3, 2014 René Reifarth 13
14 H-entrainment into He-shell flash convection zone Much higher neutron densities, since 13N get mixed deeply into the hot zones. 13C gets processed in minutes instead of 1000s of years. F. Herwig, The Astrophysical Journal 727 (2011) Oct 2-3, 2014 René Reifarth
![The i-process path Eu [Ba/Eu]~1.](/docs-images/95/123935326/images/15-0.jpg "4 Ba Nd I 15 Oct 2-3, 2014 René")
15 The i-process path Eu [Ba/Eu]~1.4 Ba Nd I 15 Oct 2-3, 2014 René Reifarth
16 Key reaction in the i-process 135 I(n,γ) Oct 2-3, 2014 René Reifarth 16
17 the p-process 35 stable neutron-deficient isotopes between 74 Se and 196 Hg Dominating reactions: (p,γ) for light nuclei; (γ,n), (γ,p), (γ,α) and β + decays for heavier nuclei Temperatures of K during time scales of a few seconds are required (type II supernovae explosions) p-nuclide r- or s- seed nuclei unstable nuclei Oct 2-3, 2014 René Reifarth 17
18 (n,γ) reactions in the p-process very high temperatures γ-induced reactions result: free neutrons and neutron-deficient material Arnould & Goriely, Physics Reports 384 (2003) 1 84 Oct 2-3, 2014 René Reifarth 18
19 Red Giants easy to spot Orion Bootes Betelgeuze Arkturus Oct 2-3, 2014 René Reifarth 19
20 Red Giants become White Dwarfs Ring nebula illuminated by the White Dwarf in the center. Oct 2-3, 2014 René Reifarth 20
21 What s needed? Neutron induced Reaction rates (1-200 kev) Neutrons Energy kev Oct 2-3, 2014 René Reifarth 21
22 Activation Method 14 C(n,g) 15 C reaction detected via 15 C(b - ) 15 N decay (t 1/2 =2.5 s) 14 C sample irradiated for 10 s, then activity counted for 10 s ( cyclic activation ) Determination of neutron flux via 197 Au(n,g) 198 Au Neutron source: 7 Li(p,n) 7 Be copper proton beam lithium Au neutron cone 14 C R. Reifarth et. al, PRC C 77, (2008) Oct 2-3, 2014 René Reifarth 22
23 A standard neutron spectrum working horse! E p =1912 kev, neutron cone fully covered Quasi-Maxwellian averaged distribution: kt = 25 kev E max = 110 kev Oct 2-3, 2014 René Reifarth 23
24 Other neutron spectra E p =1912 kev E p =2000 kev E p =2290 kev E p =2530 kev
25 15 C g-spectra
26 Description and Deconvolution p-wave capture good agreement with exp. data kev Exp. [µb] Theo. [µb] Theo/Exp
27 Neutron Captures time-of-flight technique the TOF-technique is the only generally applicable method the determine energy-dependent neutron capture cross sections beam pulsing & distance to the neutron production site significantly reduce the number of neutrons available on the sample Reifarth et al. J. Phys. G: Nucl. Part. Phys. 41 (2014) Oct 2-3, 2014 René Reifarth 27
28 The Frankfurt neutron source at the Stern-Gerlach- Zentrum (FRANZ) neutron flux: s -1 2 ma proton beam (8 A peak current) 250 khz < 1ns pulse width neutron flux at 1 m: 10 7 s -1 cm -2 neutron flux at 0.1m: 10 9 s -1 cm -2 Isotopes with half-lives down to months are in reach! Reifarth et al. PASA 26 (2009) 26, Oct 2-3, 2014 René Reifarth 28
29 NAUTILUS Neutron capture with short flightpath Increase neutron flux by factor 100 Reifarth et al. NIM A 524 (2004) Oct 2-3, 2014 René Reifarth 29
30 NAUTILUS Expected Time-Of-Flight spectrum Oct 2-3, 2014 René Reifarth 30
31 Neutron flux in astrophysical region Neutrons per second and cm 2 Oct 2-3, 2014 René Reifarth 31
32 Reaction Studies at the ESR/GSI Measurements of (p,g) or (α,g) rates in the Gamow window of the p-process in inverse kinematics in the Experimental Storage Ring. Advantages: Applicable to radioactive nuclei Detection of ions via in-ring particle detectors (low background, high efficiency) Knowledge of line intensities of product nucleus not necessary Applicable to gases Particle detectors Gas jet ESR Oct 2-3, 2014 René Reifarth 32
33 Neutron captures in inverse kinematics Neutron flux: n/cm 2 /s -> Neutron target: n/cm ions, 1 MHz: ions/s Counts per day: 20 σ / mb Reifarth & Litvinov, Phys. Rev ST Accelerator and Beams, 17 (2014) Oct 2-3, 2014 René Reifarth 33
34 Neutron capture B mv q p q const r r ( n, g ) primary 1 Same track as primary beam Reacceleration necessary electron cooler Schottky analysis determine revolution frequency Oct 2-3, 2014 René Reifarth 34
35 Schottky Analysis of revolving ions e.g. Y. A. Litvinov and F. Bosch, Rep. Prog. Phys. 74, (2011) Oct 2-3, 2014 René Reifarth 35
36 Charged-particle production, (n,2n) (n,α) : particle detectors (n,p) : particle detectors (n,2n) : particle detectors or Schottky r secondary r primary 1 Oct 2-3, 2014 René Reifarth 36
37 Fission (n,f) : only at higher energies E CM > 10 MeV Oct 2-3, 2014 René Reifarth 37
38 Possible reactions to be measured Energy regime: E n >100 kev Half live limit: t 1/2 > 0.5 h, if reactor is not pulsed Pulsed reactors might allow even smaller half-lives Oct 2-3, 2014 René Reifarth 38
39 Summary Radioactive isotopes become more and more in reach of current experimental research Neutron induced reaction studies are difficult on stable, very difficult on unstable nuclei FRANZ & NAUTILUS will push the limit further A combination of a reactor and a ion storage ring might open a new era Oct 2-3, 2014 René Reifarth 39
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