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Recent Results for proton capture S-factors from measurements of Asymptotic Normalization Coefficients R. Tribble Texas A&M University OMEG03 November,

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Presentation on theme: "Recent Results for proton capture S-factors from measurements of Asymptotic Normalization Coefficients R. Tribble Texas A&M University OMEG03 November,"— Presentation transcript:

1 Recent Results for proton capture S-factors from measurements of Asymptotic Normalization Coefficients R. Tribble Texas A&M University OMEG03 November, 2003

2 Nuclear Astrophysics Issues CNO cycle - energy producing cycle following p-p chain - important in wide range of stellar environments, including our Sun

3 CNO Cycles 13 C 13 N 12 C 14 N 15 O 15 N 17 O 17 F 16 O 18 F 18 O 19 F 20 Ne (p,  ) (p, α) (p,  ) (e +,ν) (p,  ) (p, α) (p,  ) (e +,ν) ( p,  ) (e +,ν) (p,  ) (p,α) (e +,ν) (p,α) (p,  ) IIIIII IV

4 Nuclear Astrophysics Issues CNO cycle reaction - 14 N(p,  ) 15 O (ANCs from ( 3 He,d) reaction) HCNO cycle - turns on as temperature and/or density increase - yields higher energy release, precursor to runaway

5 Na Ne F O N C 345678910 CNO Hot CNO (T 9 =0.2) Hot CNO (T 9 =0.4) Breakout Reactions http://csep10.phys.utk.edu/guidry/NC-State-html/cno.html Hot CNO Cycle and 13 N(p,  ) 14 O

6 Nuclear Astrophysics Issues CNO cycle reaction - 14 N(p,  ) 15 O (ANCs from ( 3 He,d) reaction) HCNO cycle reaction - 13 N(p,  ) 14 O (ANCs from ( 13 N, 14 O) reaction) Ne-Na cycle reaction - next cycle, 21 Ne likely source of neutrons

7 Important in second generation stars Ne – Na Cycle

8 Nuclear Astrophysics Issues CNO cycle reaction - 14 N(p,  ) 15 O (ANCs from ( 3 He,d) reaction) HCNO cycle reaction - 13 N(p,  ) 14 O (ANCs from ( 13 N, 14 O) reaction) Ne-Na cycle reaction - 20 Ne(p,  ) 21 Na (ANCs from ( 3 He,d) reaction) S 17 – yet a different measurement!

9 Direct Radiative proton capture M is: Integrate over ξ: Low B.E.: Find:

10 Radiative Capture of Charged Particle Real, ?Complex, ANC observed r>R N r<R N

11 Capture through subthreshold states well known problem for many years Subthreshold state resonance Examples: 12 C( ,  ) 16 O 13 C( ,n) 16 O 14 N(p,  ) 15 O 20 Ne(p,  ) 21 Na

12 Let us consider the radiative capture For near-threshold level, bound or resonance, assuming Coulomb plus nuclear potential Subthreshold bound state contribution behaves like resonance

13 Subthreshold Capture p radiative capture: near threshold – S matrix is: where:

14 Transfer Reaction Transition amplitude: Peripheral transfer:

15 ANC’s measured by our group stable beams 9 Be + p  10 B [ 9 Be( 3 He,d) 10 B; 9 Be( 10 B, 9 Be) 10 B] 7 Li + n  8 Li [ 12 C( 7 Li, 8 Li) 13 C] 13 C + p  14 N [ 13 C( 3 He,d) 14 N; 13 C( 14 N, 13 C) 14 N] 14 N + p  15 O [ 14 N( 3 He,d) 15 O] 16 O + p  17 F [ 16 O( 3 He,d) 17 F] 20 Ne + p  21 Na [ 20 Ne( 3 He,d) 21 Na] beams  10 MeV/u

16 S factor for 14 N(p,  ) 15 O ANC’s  14 N( 3 He,d) 15 O (d)  Rez/TAMU (27 MeV) (e)  TUNL (20 MeV) NRC to subthreshold state at E x = 6.79 MeV Subthreshold resonance width from Bertone, et al. R-Matrix fits to data from Schr ö der, et al.

17 S factor for 14 N(p,  ) 15 O C 2 (E x  6.79 MeV)  fm -1 [non-resonant capture to this state dominates S factor] S(0) = 1.40 ± 0.20 keV·b for E x  6.79 MeV S tot (0)  1.70 ± 0.22 keV·b

18 S factor dominated by direct capture to the subthreshold state Contribution from the tail of the subthreshold resonance: is negligible New reaction rate at.007 < T 9 < 0.1 lower (up to 2) than NACRE. (Impacts stellar luminosity at transition period to red giants and ages of globular clusters.) S factor for 14 N(p,  ) 15 O  width is small 

19 S factor for 20 Ne(p,  ) 21 Na Ne - Na cycle reaction Subthreshold state dominates rate 2s 1/2 at E x = 2.425 MeV,  =7.1± 0.6 keV

20 Experimental results and DWBA analysis 20 Ne( 3 He,d) 21 Na

21 present work C. Rolfs and W. S. Rodney, NPA 241, 460 (1975) Higher reaction rate for increases the abundance of and, correspondingly, the number of neutrons from    fitting parameter; new measurement would help! For subthreshold resonance (dashed line)

22 ANC’s measured by our group radioactive (rare isotope) beams 7 Be + p  8 B [ 10 B( 7 Be, 8 B) 9 Be] [ 14 N( 7 Be, 8 B) 13 C] 11 C + p  12 N [ 14 N( 11 C, 12 N) 13 C] 13 N + p  14 O [ 14 N( 13 N, 14 O) 13 C] 17 F + p  18 Ne [ 14 N( 17 F, 18 Ne) 13 C] {ORNL (TAMU collaborator)} beams  10 - 12 MeV/u

23 13 N(p,  ) 14 O D.Decrock et al., PRC48, 2057(1993)

24 ANC’s for 13 N + p  14 O reaction: 14 N( 13 N, 14 O) 13 C K500: 13 C beam  195 MeV MARS: 13 N beam  153 MeV

25 14 N( 13 N, 14 O) 13 C C 2 = 29.0 ± 4.3 fm -1 DWBA by FRESCO ( ANC for p)p) CN  1314

26 S Factor for 13 N(p,  ) 14 O DC/Decrock_dc = 1.4 Constructive/Decrock_tot =1.4 Constructive/Destructive =4.0 ( expected constructive interference for lower energy tail, useful to check) For Gamow peak at T 9 =0.1,

27 Transition from CNO to HCNO Transition from CNO to HCNO 13 N(p,  ) 14 O vs  decay 14 N(p,  ) 15 O vs  decay Crossover at T 9   0.2 For novae find that 14 N(p,  ) 15 O slower than 13 N(p,  ) 14 O; 14 N(p,  ) 15 O dictates energy production X H =0.77

28 ANC’s measured by our group stable beams (mirror symmetry) 7 Be + p  8 B [ 13 C( 7 Li, 8 Li) 12 C] 22 Mg + p  23 Al [ 13 C( 22 Ne, 23 Ne) 12 C] [underway now]

29 ANC’s for 7 Be + p  8 B from mirror reaction 13 C( 7 Li, 8 Li) 12 C separate p 1/2 and p 3/2 Fits  ANC’s 7 Li + n   Li: C 2 (p 3/2 ) =.384±.038 fm -1 C 2 (p 1/2 ) =.048±.006 fm -1  7 Be + p   B: C 2 (p 3/2 ) =.405±.041 fm -1 C 2 (p 1/2 ) =.050±.006 fm -1 p 1/2 p 3/2 S 17 (0) = 17.6±1.7 eVb

30 Collaborators TAMU: A. Azhari, H. Clark, C. Gagliardi, Y.-W. Lui, A. Sattarov, X. Tang, L. Trache, A. Zhanov INP (Czech Republic): V. Burjan, J. Cepjek, V. Kroha, J. Piskor, J. Vincour IAP (Romania): F. Carstoiu

31 TAMU Upgrade Plans Further develop RIB capability Produce accelerated RIB’s at intermediate energies [white paper at http://cyclotron.tamu.edu/]

32

33 TAMU Upgrade Plans Stage I - commission K150(88”) cyclotron - ECR source injection - commission beam lines to existing apparatus Stage II - isotope production stations completed - production of rare isotopes Stage III - K500 acceleration of rare isotope beams

34 Proposed Layout

35 TAMU Upgrade Stage I – Performance K150 beams IsotopeEI EI MeV/upApA pApA p5027 20 Ne263 d3020 22 Ne240.5 3 He4010 34 S180.7 4 He3010 40 Ar161.4 6 Li307 40 Ca161.5 7 Li228 59 Co100.9 10 B304 78 Kr90.6 11 B245 86 Kr80.6 16 O302 129 Xe5.60.5 (Simultaneous operation of K150 and K500 into different experimental areas.)

36 TAMU Upgrade Stage II and III Couple IG (light ion beams) and HI target stations to K150 Complete 1 +  n + ECR source Begin Rare Ion production

37 TAMU Upgrade Stage III Performance Ion Guide (heavy ions) into K500 Isotope Max. EnergyIntensity Mev/upps 9 Li453 x 10 6 12 Be455 x 10 6 38 S365 x 10 5 44 S262 x 10 2 42 Ar397 x 10 5 62 Fe384 x 10 4 8B8B702 x 10 6 14 O631 x 10 5 22 Mg576 x 10 4 27 P622 x 10 3 62 Ga474 x 10 2 64 Ga452 x 10 4 neutron-rich isotopes proton-rich isotopes

38 TAMU Upgrade Plans Cost  $4 M Proposal submitted - 12/1/03 Time line  2 years for stage I - II  2 more years for completion and first experiment

39 Check for Peripheral Transfer d  /d  as function of radial cutoff localization of angular momentum transfer vary r and a in Wood-Saxon well i.e.  vary b

40 30  cm (deg) 01020405060.1.01 1. d  /d  ( mb/sr ) 3/2 -, 6.18 MeV 30  cm (deg) 01020405060 d  /d  ( mb/sr ).1 1. 10. 1/2 -, 0.0 MeV 14 N( 3 He,d) 15 O

41 Fates of Massive Pop III Stars G 33 H G pp-I,II,III H G CNO, rp Collapse Black Hole Explode Metallicity=(X A /X H )/(X A /X H ) sun 3   sufficient 12 C for M < 5x10 5 M sun metallicity(Z)  5x10 -5 to explode

42 Updated Reaction Sequences in Pop III Stars Rap-I,II and III, substitution for 3  and CNO! (Wiescher et al., 1989)

43 Asymptotic Normalization Constant Both tails dominated by Coulomb interaction->same solution ANC describes the absolute magnitude of the tail of the overlap function and is determined by the complicated internal n-n interaction b lj, obtained with potential model, strongly depends on geometric parameters

44 Recent Results for proton capture S-factors from measurements of Asymptotic Normalization Coefficients R. Tribble Texas A&M University OMEG03 November, 2003

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