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Indirect Techniques ( I) : Asymptotic Normalization Coefficients and the Trojan Horse Method NIC IX R.E. Tribble, Texas A&M University June, 2006
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Why use Indirect Techniques? Reaction rates on radioactive nuclei Capture through subthreshold states Direct capture to add to resonant capture Screening and low-energy extrapolations Get cross sections difficult for direct studies! Including:
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Some Indirect Techniques [focus on reaction rates] Widths ( and ‘p’) of resonance rates - populate resonance state and measure decay Resonance energies – determine E R Coulomb dissociation Trojan Horse Method - unique way to understand screening Asymptotic Normalization Coefficients - use with stable and radioactive beams ** (T. Motobayashi) **Experts in audience for detailed questions! } resonant capture
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Radiative [p( )] Capture with resonant and subthreshold states: ANCs subthreshold state resonance Capture through resonance
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Radiative [p( )] Capture with resonant and subthreshold states: ANCs subthreshold state resonance Direct capture
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Radiative [p( )] Capture with resonant and subthreshold states: ANCs subthreshold state resonance Capture to ground state through subthreshold state
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Measuring ANCs: Transfer Reactions Transition amplitude: Peripheral transfer: [S = C 2 /b 2 ]
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ANC Examples: capture at stellar energies DC: 7 Be(p, ) 8 B and 7 Be + p 8 B 22 Mg(p, ) 23 Al and 22 Ne + n 23 Ne DC through subthreshold state: 14 N(p, ) 15 O and 14 N + p 15 O 13 C( ,n) 16 O and 13 C + 17 O (2 posters) DC and resonance interference: 13 N(p, ) 14 O and 13 N + p 14 O
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S factor dominated by direct capture—our published value via ANCs from two ( 7 Be, 8 B) transfer reaction studies: S(0) = 18.0 1.9 eV b Result low by about 2 compared to most recent direct measurement (?) Details about 7 Be(p, ) 8 B from C.D. in later talk S factor for 7 Be(p, ) 8 B
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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
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S factor for 14 N(p, ) 15 O some preliminary results C 2 (E x 6.79 MeV) fm -1 [non-resonant capture to this state dominates S factor] S(0) 1.41 ± 0.24 keV·b for E x 6.79 MeV S tot (0) 1.62 ± 0.25 keV·b Subthreshold state: slide from NIC VII
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S factor dominated by direct capture to the subthreshold state—our published value S(0) = 1.62 0.25 keV b reduces previous results by 2 New direct measurements from LUNA (1.7±0.2) and LENA (1.68±0.09±0.16) in excellent agreement with this Impacts stellar luminosity at transition period to red giants and ages of globular clusters by about 1 Gyr S factor for 14 N(p, ) 15 O
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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
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14 N( 13 N, 14 O) 13 C DWBA by FRESCO (ANC for p)p) CN 1314 C 2 = 29.0 ± 4.3 fm -1
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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, Preliminary
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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
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S factor dominated by subthreshold state ( E x =6.356 MeV) S factor for 13 C( ,n) 16 O and s-process neutrons ANC from 6 Li( 13 C,d) 17 O – sub Coulomb transfer (recent result from Florida State University and TAMU, earlier result - Kubono) ANC + n gives S(0) = 2.36 0.52 10 6 Mev b Factor of 10 below present NACRE value [posters on this topic!]
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S factor dominated by direct capture up to T 9 0.2 S factor for 22 Mg(p, ) 23 Al 22 Mg produced in ONe novae in Ne-Na cycle source of 22 Na decay or p capture dominate? Use charge symmetry for ANC: -decay of 23 Al gnd. state is 5/2 +
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22 Mg (p, ) 23 Al Reaction Rate E C.M [MeV] S -factor [KeV b] T 9 (10 9 K) S(E) – Direct Capture reaction rate ρ=10 6 gm/cm 3, T 9 =0.4 22 Mg(p, ) 23 Al competes with β + rate but photodisintegration is issue Reaction Rate (cm 3 /mole/s)
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Charged Particle Capture: the Trojan Horse Method I Many charged-particle reaction rates important in stellar evolution Laboratory measurements Coulomb barrier issues (e.g. electron screening) making extrapolation difficult THM (Baur – 1986) uses surrogate to remove Coulomb effects
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THM - Example Consider a reaction 6 Li(d, ) 4 He THM use 6 Li( 6 Li, ) 4 He d spectator 6 Li( 6 Li, ) 4 He for 6 Li(d, ) 4 He THM - Spitaleri et al. Direct data Englster et al. 6 Li
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Charged Particle Capture: the Trojan Horse Method II Issues: – transferred particle is off energy shell – initial and final state effects important – no absolute normalization – must have quasi-free kinematics – analysis with PWIA and MPWIA
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Some Reaction Mechanism Issues Coulomb effects included [Mukhamedzhanov et al., nucl/th-0602001] Three calculations (spectator ignored) as a function of =(p d ) 2 /( d ) 2 ‘on shell’ transfer =0 (black) ‘half off shell’ with QF kinematics =m +m d -m Li = BE (red) ‘half off shell’ with = 1.5 BE (blue) 6 Li + 6 Li + + for Final state effects also not important!
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THM Applications Direct Capture: – extrapolation to S(0) without e-screening – extraction of screening potential Resonant capture: – extrapolation to S(0) with small uncertainty Subthreshold Capture: – observe effects at very low relative energy
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U e (ad) U e (Dir) 6 Li+d 186 eV330 ± 120 eV U e (ad) U e (Dir) 6 Li+p 186 eV440 ± 80 eV U e (ad) U e (Dir) 7 Li+p 186 eV300 ± 160 eV 7 Li + p + S 0 =55 3 keV b 6 Li + d + S 0 = 16.9 MeV b 6 Li+p + 3 He So = 3 0.9 MeVb 6 Li+d + 7 Li+p + 6 Li+p + 3 He R-matrix calculation direct data From C.S. Direct Capture
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9 Be(p, ) 6 Li reaction 2 H( 9 Be, 6 Li)n The 9 Be(p, ) 6 Li reaction via 2 H( 9 Be, 6 Li)n Laboratory: Tandem: LNS INFN-Catania Energy: E 9Be = 22 MeV 2H2H p 9 Be n 6 Li α I II THM Direct data Reaction important for depletion of light nuclei From C.S. Resonant Capture
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The 15 N(p, ) 12 C reaction via d( 15 N, 12 C )n 2H2H p n α I II 15 N 12 C Destroys 15 N reduces 19 F production in AGB stars From C.S. Laboratory: TAMU (K500 cyclotron) 2 H( 15 N, 12 C)n E beam = 60 MeV S(0) 37 MeVb [about 1/2 NACRE value] Preliminary
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Summary Indirect techniques valuable tools in N.A. Useful for range of reaction types S(0) with different extrapolation systematics Can provide auxiliary information Yield cross sections difficult to get otherwise! Challenge for the future: find new techniques to understand (n, ) rates
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Collaborators ANCs: T. Al-Abdullah, A. Azhari, A. Banu, P. Bem, V. Burjan, F. Carstoiu, C. Fu, C. Gagliardi, V. Kroha, J. Piskor, A. Sattarov, E. Simeckova, G. Tabacaru, X. Tang, L. Trache, J. Vincour, Y. Zhai, A. Mukhamedzhanov THM (TAMU experiment) : C. Spitaleri,S. Cherubini, V. Crucilla, M. La Cognata, L. Lamia, R.G. Pizzone, S. Romano, A. Tumino
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