1. Astrophysical p-process: the synthesis of heavy, proton-rich isotopes Gy. Gyürky Institute of Nuclear Research (ATOMKI) Debrecen, Hungary Carpathian Summer School of Physics 2012, June 24 – July 7, 2012, Sinaia, Romania

2. 2 Composition of the Solar System Big bang, H, He, ( 7 Li) Cosmic ray, Li, Be, B Stellar burning stages, C-Fe Heavy elements: s-, r-, p-processes, Fe-U

3. Synthesis of elements heavier than Iron No energy generation above Iron Increasing Coulomb barrier  low charged particle induced cross section High Coulomb barrier cannot be overcome by increasing temperature (  -induced reactions become faster)  Charged particle induced reactions cannot play the key role 3

4. 4 Heavy element nucleosynthesis

5. 5 s-process n capture  - decay  + decay

6. 6 Heavy element nucleosynthesis r-process n capture  - decay  + decay

7. 7 Heavy element nucleosynthesis r-process p-isotopes p-process n capture  - decay  + decay

8. 8 p-nuclei (p-nuts) 74 Se 78 Kr 84 Sr 92 Nb 92,94 Mo 96,98 Ru 102 Pd 106,108 Cd 113 In 112,114 Sn 120 Te 124,126 Xe 130,132 Ba 138 La 136,138 Ce 144,146 Sm 156,158 Dy 162 Er 168 Yb 174 Hf 180 Ta 180 W 184 Os 190 Pt 196 Hg mainly even-even nuclei 0.1-1% isotopic abundance Abundance information only from the Solar System

9. The synthesis of p-nuclei … rp-process  -process

10. rp-process (rapid proton capture) 10 High temperature, proton rich environment, consecutive proton captures and β-decays  Explosive H burning, breakout from the hot CNO cycle Primary process Site: Accreting neutron star, X-ray burst (and others suggested)

11. Problems with the rp-process Definite endpoint around the alpha emitter Te isotopes The created isotopes are trapped on the surface of the neutron star 11 H. Schatz et al. Phys. Rev. Lett. 86, 3471 (2001) SnSbTe cycle

12. 12 116 Sn 115 Sn 114 Sn 113 Sn 112 Sn 111 Sn 110 Sn 109 Sn 106 Cd 108 Cd ( ,n) (,)(,) ( ,p) 108 Sn The gamma-process Gamma-induced /mainly ( ,n)/ reactions on s- and r-process seed isotopes Secondary process

13. 13 gamma-process reaction network ~ 2000 isotopes ~ 20000 reactions Mainly ( ,n), ( ,  ), ( ,p) reaction and beta decays The models are not able to reproduce the observed p-isotope abundances T. Rauscher et al. Rep. Prog. Phys. in prep

14. Possible explanations 14 Other processes may contribute:  rp-process  -process  p-process  pn-process  … Problems with astrophysical input Problems with nuclear physics input

15. Astrophysics input: site and conditions  -induced reactions with Planck photons: high temperature needed (GK range) Necessary seed nuclei must be available Time scale: not too short, not too long (~1s) 15 Preferred site: O/Ne layers of massive stars in type II supernova explosions

16. Nuclear physics input Nuclear masses (rather well known) Decay properties Reaction rates (obtained from cross sections)  Thousands of reactions  Mainly gamma-induced  Typically taken from theory: Hauser-Feshbach statistical model  Calculated p-isotope abundances are (very) sensitive to (some) reaction rates 16 Experimental determination of the relevant cross sections is necessary

17. Gamma-induced reactions Experimental investigation is challenging (fast progress, though: bremsstrahlung, inverse Compton scattering, Coulomb dissociation) Effect of thermally excited states on the reaction rate is more important for  -induced reactions Detailed balance: direct relation between (x,  ) and ( ,x) reaction rate 17  capture reactions should be studied

18. Capture reaction cross section measurement Large database for (n,  ) reaction Very few data for ( ,  ) and (p,  ) 18 ( ,  ) reactions Need for ( ,  ) and (p,  ) data!!!

19. 19 Experimental challenges Relevant energy range (Gamow window): (p,  ): 1-4 MeV (Coulomb barrier: 7-12 MeV) ( ,  ): 5-15 MeV (Coulomb barrier: 10-20 MeV)  low cross section Compound nucleus with overlapping levels  complicated decay scheme (many transitions) The conventional in-beam gamma-spectroscopy is difficult See the talk of Artemis Spyrou! 88 Sr(p,  ) 89 Y

20. 20 Activation method Cons: The final nucleus must be radioactive (and the half-life must be appropriate) Some radiation with sufficient intensity is needed Pros: Much cleaner  -spectra Isotropic angular distribution More isotopes studied simultaneously Activity N o 84 Sr(p,  ) 85 Y 86 Sr(p,  ) 87 Y 87 Sr(p,  ) 88 Y

21. 21 Experiments at ATOMKI Alpha-induced reactions: 5-15 MeV  Cyclotron Proton-induced reactions: 1-4 MeV  Van de Graaff http://www.atomki.hu/

22. 22 Capture reaction cross section measurements

23. 23 Results Cross section measured at energies as low as possible  (p,  ) reaction: in the Gamow window  ( ,  ) reaction: above the Gamow window Comparison with statistical model calculations Reaction rates, astrophysical consequences

24. 24 Comparison with theory 130 Ba( ,  ) 134 Ce Z. Halász et al., Phys. Rev. C 85 (2012) 025804.

25. Input for statistical models The statistical model uses input parameters  Reaction Q values (masses)  Ground and exited state properties  Level densities  Gamma-ray strength functions  Optical model potentials The resulting cross sections strongly depend on them 25

26. 26 Dependence on input parameters 106 Cd( ,  ) 110 Sn Gy. Gyürky et al., Phys. Rev. C 74 (2006) 025805

27. 27 Fine tuning of parameters G.G. Kiss et al., Phys. Rev. Lett. 101 (2008) 191101

28. 28 Fine tuning of parameters G.G. Kiss et al., Phys. Rev. Lett. 101 (2008) 191101 Imaginary potential strength increased by 70%

29. 29 Alpha-nucleus optical potential E. Somorjai et al., A&A 333 (1998) 1112. 144 Sm( ,  ) 148 Gd

30. 30 Direct determination of alpha-nucleus optical potential High precision elastic scattering experiments Low energies (around Coulomb-barrier) Comparison with global optical potentials Construction of local potentials Experiments: cyclotron of ATOMKI

31. 31 Capture and scattering experiments

32. 32 Measured complete angular distributions G.G. Kiss et al., Phys. Rev. C 80 (2009) 045807

33. 33 Dependence on proton or neutron number

34. 34 Construction of local potentials

35. ( ,  ) vs. ( ,  ) 35 112 Sn( ,  ) 116 Te See the talk of V. Avrigeanu next Tuesday!

36. 36 106 Cd 108 Cd 110 Cd 108 Sn 110 Sn 112 Sn 114 Sn (,)(,) (,)(,) (,)(,) ( ,n) ( ,p) old new secondary paths T = 2.0·10 9 K reaction rates Direct influence on  -process networks Main reaction path based on the

37. Novel methods Activation experiments: limited to radioactive product isotopes Direct in-beam measurements: limited to stable targets  -process network: reactions on radioactive isotopes also play a role  Can be studied with RIB facilities 37

38. Example: storage ring experiment 38 96 Ru(p,  ) 97 Rh reaction in inverse kinematics at ESR, GSI

39. Summary and conclusions p-isotope production: one of the least understood processes of nucleosynthesis Experiments are necessary:  Gamma-induced reactions  Capture reactions  Elastic scattering New experimental techniques are also necessary 39

40. Thank you for your attention! 40 P-nut