Credit: NASA/CXC/M.Weiss
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2 Credit: NASA/CXC/M.Weiss Hydrogen and helium (Li,B, Be) from the Big-Bang nucleosynthesis, everything else from stellar processes [e.g. C. Iliadis, Nuclear Physics of Stars, Wiley-VCH Verlag, Weinheim (2007)] 2
3 Credit: NASA/CXC/M.Weiss Hydrogen and helium (Li,B, Be) from the Big-Bang nucleosynthesis, everything else from stellar processes [e.g. C. Iliadis, Nuclear Physics of Stars, Wiley-VCH Verlag, Weinheim (2007)] 3
4 Image from pixabay.com but free neutrons are perishables (mean lifetime 15 min) [M. Arnould, S. Goriely, and K.Takahashi, Phys. Rep. 450, 97 (2007)] 4
5 Direct evidence: spectral lines from technetium in red giant stars -> Tc has no stable isotopes, 99 Tc produced by b - decay of 99 Mo [P. W. Merrill, Astrophys. J. 116, 21 (1952)] Cat s Eye nebula (credit:nasa) The s-process path follows the valley of stability -> most cross sections are measured except branch points [Käppeler et al., Rev. Mod. Phys. 83, 157 (2011)] 5
![119, 1611 (2017)] [D. Kasen et al.](/docs-images/82/85445679/images/6-3.jpg ", Nature 551, 80 (2017)] and many more [Figure from Prof.")
![Stephane Goriely s talk at the 13 th Nordic Meeting on Nuclear Physics, 2015]](/docs-images/82/85445679/images/6-5.jpg "Prompt merger ejecta are cold -> no (n,g)-(g,n) equilibrium -> (n,g) reaction")
6 Detection of a neutron star collision 17 Aug 2017 by LIGO & Virgo Finally one confirmed site for the r-process! [B.P. Abbott et al., Phys. Rev. Lett. 119, 1611 (2017)] [D. Kasen et al., Nature 551, 80 (2017)] and many more [Figure from Prof. Stephane Goriely s talk at the 13 th Nordic Meeting on Nuclear Physics, 2015] Prompt merger ejecta are cold -> no (n,g)-(g,n) equilibrium -> (n,g) reaction rates matter [M. Arnould, S. Goriely and K. Takahashi, Phys. Rep. 450, 97 (2007)] 6
![Phys. 76, 066201 (2013)]](/docs-images/82/85445679/images/7-2.jpg "Favorable astrophysical sites:")
7 Credits: ESA/Hubble & NASA [Rauscher et al., Rep. Prog. Phys. 76, (2013)] Favorable astrophysical sites: Explosive O-Ne shell burning of type II supernovae, type Ia supernovae, Secondary process peeling off neutrons on existing heavy nuclei 7
8 What s the chance for or Opticalmodel potential Level density Uncertain input Uncertain output Gammadecay strength # 8 & N A σ v (T ) = % ( $ πm ' 1/2 N A (kt ) 3/2 G(T ) 0 G(T ) = (2I µ +1) / (2I 0 +1)exp( E x µ / kt ) µ µ (2I µ +1) (2I 0 +1) σ * µ (E)E exp (E + E x, + kt µ ) - / de. 8
9 44 Sc data E x 0 6- I 0. Get a hold of an (Eg,Ex) matrix (> coincidences) 1. Correct for the NaI response [Guttormsen et al., NIM A 374, 371 (1996)] 2. Extract distribution of primary g s for each Ex [Guttormsen et al., NIM A 255, 518 (1987)] 3. Get level density and g-strength from primary g s [Schiller et al., NIM A 447, 498 (2000)] 4. Normalize & evaluate systematic errors [Schiller et al., NIM A 447, 498 (2000), Larsen et al., PRC 83, (2011)] 9
10 44 Sc data E x 0 6- I 0. Get a hold of an (Eg,Ex) matrix (> coincidences) 1. Correct for the NaI response [Guttormsen et al., NIM A 374, 371 (1996)] 2. Extract distribution of primary g s for each Ex [Guttormsen et al., NIM A 255, 518 (1987)] 3. Get Data level and density references: and g-strength from primary g s [Schiller et al., NIM A 447, 498 (2000)] 4. Normalize & evaluate systematic errors [Schiller et al., NIM A 447, 498 (2000), ocl.uio.no/compilation/ Analysis codes and tools: github.com/oslocyclotronlab/oslo-method-software Larsen et al., PRC 83, (2011)]
11 CACTUS: 26 collimated NaI(Tl) crystals, 5 x 5 SiRi: 8x8 Si ΔE-E particle detectors ( 9% of 4π) 11
12 CACTUS: 26 collimated NaI(Tl) crystals, 5 x 5 SiRi: 8x8 Si ΔE-E particle detectors ( 9% of 4π) NaI(Tl) 3 He a o Si DE-E telescope Target nucleus 12
13 CACTUS: 26 collimated NaI(Tl) crystals, 5 x 5 SiRi: 8x8 Si ΔE-E particle detectors ( 9% of 4π) NaI(Tl) 3 He New g-ray detector system in progress (30 LaBr x 8 crystals) [Funding from NFR] Target nucleus a o Si DE-E telescope 13
14 14
15 15
16 94 Mo(d,pgg) 95 Mo ) -3 γ-ray strength function (MeV Fe( He,αγ), Voinov et al. Fe(p,p γ), NaI:Tl Fe(p,p γ), LaBr :Ce 3 Co(γ,n), Alvarez et al γ-ray energy E (MeV) γ Confirmed with an independent technique using (d,pgg) coincidences [M. Wiedeking et al., PRL111, (2013)] x 8 LaBr 3 (Ce) from the HECTOR + array Dominated by dipole transitions [A.C. Larsen et al., PRL 111, (2013)] Heaviest case with upbend so far: 151,153 Sm [Simon et al., PRC 93, (2016)] Small bias towards M1: Jones et al., PRC 97, (2018) 16
17 94 Mo(d,pgg) 95 Mo ) -3 γ-ray strength function (MeV Fe( He,αγ), Voinov et al. Fe(p,p γ), NaI:Tl Fe(p,p γ), LaBr :Ce 3 Co(γ,n), Alvarez et al γ-ray energy E (MeV) γ Confirmed with an independent technique using (d,pgg) coincidences [M. Wiedeking et al., PRL111, (2013)] x 8 LaBr 3 (Ce) from the HECTOR + array Dominated by dipole transitions [A.C. Larsen et al., PRL 111, (2013)] Heaviest case with upbend so far: 151,153 Sm [Simon et al., PRC 93, (2016)] Small bias towards M1: Jones et al., PRC 97, (2018) 17
18 1. Unexpected experimental result new decay mode? 2. Impact on r-process reaction rates? Rate <σv> (upbend)/rate (GLO-up2)/<σv> (no upbend) (GLO) Reaction = 1 GK TALYS: Koning et al., Fe N Mo but is the upbend really there for n-rich nuclei? Cd [A.C. Larsen and S. Goriely, Phys. Rev. C 82, (20)] 18
19 Branch-point nuclei 185 W, 186 Re, 191 Os (ERC gresonant) 191 Ir 186 Os 187 Os 188 Os 189 Os 190 Os 191 Os 192 Os 185 Re 186 Re 187 Re s-process flow 3.78d (n,g) 183 W 184 W 185 W 186 W 74.8d r-process flow 19
20 Branch-point nuclei 185 W, 186 Re, 191 Os (ERC gresonant) Proof-of-principle, Zr region [Guttormsenet al., PRC 96, (2017)] 191 Ir 186 Os 187 Os 188 Os 189 Os 190 Os 191 Os 192 Os MSc thesis, Ina Kullmann (2018): First experimental constraint on the Re 186 Re 187 Os(n,g) reaction Re s-process flow 3.78d (n,g) 183 W 184 W 185 W 186 W 74.8d r-process flow 20
21 Young, Talented Researcher Grant, Research Council of Norway: Dr. Gry Merete Tveten, SNAPS 92 Mo is typically underproduced by 1 2 orders of magnitude. [Tveten et al., PRC 94, (2016)] 21
22 Young, Talented Researcher Grant, Research Council of Norway: Dr. Gry Merete Tveten, SNAPS 92 Mo is typically underproduced by 1 2 orders of magnitude. Based on our results, we conclude that the 92 Mo abundance anomaly is not due to the nuclear physics input to astrophysical model calculations. [Tveten et al., PRC 94, (2016)] 22
23 NSCL/Michigan State University summer 2014 Advantage: can go down to implantation rate of 1 pps J 1) Implant a neutron-rich nucleus inside a segmented total-absorption spectrometer 2) Measure b-particle in coincidence with all g rays from the daughter nucleus (kev) 7000 Unfolded spectra, 76 Ga beta-decaying to 76 Ge 4 E x Segmented, total absorption spectrometer SuN [A. Simon, S.J. Quinn, A. Spyrou et al, NIM A 703, 16 (2013)] (kev) E γ 23 1
24 NSCL/Michigan State University summer 2014 Advantage: can go down to implantation rate of 1 pps J 1) Implant a neutron-rich nucleus inside a segmented total-absorption spectrometer 2) Measure b-particle in coincidence with all g rays from the daughter nucleus (kev) 7000 Unfolded, 76 Ge 4 E x Segmented, total absorption spectrometer SuN [A. Simon, S.J. Quinn, A. Spyrou et al, NIM A 703, 16 (2013)] (kev) E γ 24 1
25 NSCL/Michigan State University summer 2014 Advantage: can go down to implantation rate of 1 pps J 1) Implant a neutron-rich nucleus inside a segmented total-absorption spectrometer 2) Measure b-particle in coincidence with all g rays from the daughter nucleus (kev) 7000 Unfolded, 76 Ge 4 E x Segmented, total absorption spectrometer SuN [A. Simon, S.J. Quinn, A. Spyrou et al, NIM A 703, 16 (2013)] (kev) E γ 25 1
26 Discretionary beam NSCL/MSU, February 2015; 70 Co beta-decaying into 70 Ni (Spokespersons: Sean Liddick, Artemis Spyrou, ACL & Magne Guttormsen) 86 Kr primary beam, 140 MeV/nucleon on thick Be target 70 Co implanted on DSSD detector in SuN 70 Co T 1/2 : 5 ms, I p = 6 -, Q b = 12.3 MeV S n of 70 Ni: 7.3 MeV Initial spins, 70 Ni (Gamow-Teller): 5 -,6 -,7 - [S.N. Liddick A. Spyrou, B.P. Crider, F. Naqvi, A.C. Larsen, M. Guttormsen et al., Phys. Rev. Lett. 116, (2016)] 26
27 Discretionary beam NSCL/MSU, February 2015; 70 Co beta-decaying into 70 Ni (Spokespersons: Sean Liddick, Artemis Spyrou, ACL & Magne Guttormsen) 86 Kr primary beam, 140 MeV/nucleon on thick Be target 70 Co implanted on DSSD detector in SuN 70 Co T 1/2 : 5 ms, I p = 6 -, Q b = 12.3 MeV S n of 70 Ni: 7.3 MeV Initial spins, 70 Ni (Gamow-Teller): 5 -,6 -,7 - [S.N. Liddick A. Spyrou, B.P. Crider, F. Naqvi, A.C. Larsen, M. Guttormsen et al., Phys. Rev. Lett. 116, (2016)] 27
28 Discretionary beam NSCL/MSU, February 2015; 70 Co beta-decaying into 70 Ni (Spokespersons: Sean Liddick, Artemis Spyrou, ACL & Magne Guttormsen) Kr primary beam, 140 MeV/nucleon Ni(n,γ) Ni rate on thick Be target 70 Co implanted on DSSD detector in SuN ) -1 BRUSLIB JINA REACLIB s -1 mol 70 Co T 1/2 : 5 ms, I p = 6 -, Q b = 12.3 MeV S n of 70 Ni: 7.3 MeV Initial spins, 70 Ni (Gamow-Teller): 5 -,6 -,7-3 (cm N A σv T ( 9 K) [S.N. Liddick A. Spyrou, B.P. Crider, F. Naqvi, A.C. Larsen, M. Guttormsen et al., Phys. Rev. Lett. 116, (2016)] 28
29 (a) (b) (c) Ex (MeV) Ex (MeV) Ex (MeV) E g (MeV) E g (MeV) E g (MeV) 0 0 [Larsen, Midtbø, Guttormsen, Renstrøm et al., PRC 97, (2018)] 29
30 (a) (b) (c) Ex (MeV) Ex (MeV) Ex (MeV) E g (MeV) E g (MeV) E g (MeV) 0 0 [Larsen, Midtbø, Guttormsen, Renstrøm et al., PRC 97, (2018)] 30
31 (a) (b) (c) f (MeV 3 ) E g (MeV) Shell-model calculations by Jørgen E. Midtbø using KSHELL [Shimizu, arxiv: ] Ex (MeV) E g (MeV) Ex (MeV) 56 Ni 57 Ni 58 Ni 59 Ni 60 Ni 61 Ni 62 Ni E g (MeV) 63 Ni Ex (MeV) 65 Ni 66 Ni 67 Ni 68 Ni 69 Ni 70 Ni 72 Ni 74 Ni Ni 76 Ni E g (MeV) [Larsen, Midtbø, Guttormsen, Renstrøm et al., PRC 97, (2018)] 31
32 Accepted experiment proposal (2018 call): The rare-earth r-process peak: Sm(n,g) reaction rates constrained with the beta-oslo method From Mumpower et al., PRC 86, (2012) 32
33 Accepted experiment proposal (2018 call): The rare-earth r-process peak: Sm(n,g) reaction rates constrained with the beta-oslo method Future possibilities for beta-oslo method type experiments at FAIR, GANIL, SPES, Jyvaskyla,? From Mumpower et al., PRC 86, (2012) 33
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