Nuclear Astrophysics at the ISAC Radioactive Beams Facility: Prelude for RIA

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1 Nuclear Astrophysics at the ISAC Radioactive Beams Facility: Prelude for RIA John D Auria for the DRAGON Collaboration Radioachemistry at RIA Symposium 225 th National ACS Meeting, New Orleans March 27, 2003

2 RIA is intended to be next generation RB facility producing with much higher intensites and perhaps purities. A key factor in designing it properly is to know what you wish to do with it and to learn from what has been developed in the past. It is important that it be appreciated that RIA is NOT starting from scratch. The purpose of this talk is to inform you about what we are doing with ISAC, the premier RB facility today generally in various areas of science and specifically in the area of nuclear astrophysics. I will use the first successful experiment performed with DRAGON using RB as an example to illustrate what we have learned working with RB at ISAC.

3 Outline Radioactive Beams and ISAC Experimental Facilities at ISAC TUDA and DRAGON The 21 Na(p,γ) 22 Mg Reaction Motivation, Experiment, Results Future Plans (DRAGON and ISAC) Concluding Remarks and Suggestions

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5 Production of Radioactive Beams RIA ISAC

6 The TRIUMF-ISAC Radioactive Beams Facility ISAC Project proposed in 1985 ISAC Project funded in 1995 RB Production by the ISOL Method RB Accelerated using LINACS ( MeV/u) Two Experimental Areas (LEBT and HEBT) Major Milestones 1998 First RB beam ( 38m K) to TRINAT 2000 First physics ( 74 Rb lifetime with high precision) ISAC II funded 2001 TUDA and DRAGON perform RB experiments π and β-nmr perform physics TITAN and TIGRESS FUNDED

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10 Radioactive Beams at TRIUMF The ISOL Method M. Dombsky TRIUMF MeV protons onto thick target Have used Nb, Ta, SiC, TiC, CaO, CaZrO 3, (ZrC) Intensities up to 100 µa possible (now 40 µa) Products diffuse out at high temperatures Species ionized in surface ion source; ECR (2003); Laser(2004) Some Beam Intensities at Yield Station 8 Li (Ta) 8 x 10 8 pps 11 Li (Ta) 2 x 10 4 pps 21 Na (SiC) 9.9 x 10 9 pps 74 Rb (Nb) 1.3 x 10 4 pps 79 Rb (Nb) 4.6 x 10 9 pps 160 Yb (Ta) 8.4 x 10 9 pps

11 ISAC I Science Program ISAC 1 Facilities Nuclear Astrophysics Fundamental Symmetries Condensed Matter Physics Nuclear Structure DRAGON TUDA TRINAT GPS LTNO Beta NMR 8π Gamma array RT Collection Station OSAKA Systems

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13 [TRINAT] Collection Facility Separator floor

14 ISAC LINACS Energy: MeV/u Pulse Iteration: 86 ns Masses: A < 30 amu

15 TUDA - TRIUMF University of Edinburgh Detector Array 21 Na(p,p ) PRC 65 (2002) Na(p,p ) L. Buchmann TRIUMF P. Walden TRIUMF

16 Highly-Segmented 4π Si Array (TUDA-II) TUDA at ISAC-I Transfer Reactions in inverse kinematics with accelerated radioactive beams from ISAC-II.

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18 Aims of Nuclear Astrophysics Understand the origin and evolution of the chemical elements Understand the nuclear processes responsible for energy generation light curve of X-ray burst MXB HEAO

19 The Big Picture

20 Explosive Astrophysical Sites Novae, X-ray bursters, supernovae type 1a Binary system compact object and main sequence or red giant star Accretion of hydrogen rich material Thermonuclear runaway lots of energy High temperatures and short timescales Radioactive nuclei important

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22 Explosive Nucleosynthesis in ONeMg-Novae Present Understanding H rich material accumulates on surface of white Dwarf that had underwent C-burning in prior life T < 0.4 GK too low for rp breakout ρ ~ 10 g/cm source of thermonuclear runaway: NeNa cycle Nova Cygni Erupted 2/92 Left 5/93 Right 6/94

23 Astrophysical Interest in 21 Na(p,γ) 22 Mg 21 Na(p,γ) 22 Mg Reaction plays an important role in the abundance of 22 Na in expelled material. Presence of 22 Na can be measured through observation of 1.28 MeV decay gamma. (COMPTEL, INTEGRAL) For Novae Her1991 and Cyg1992 only upper limits on 22 Na abundance were detected, well below expected value at this time. Observation of 1.28 MeV gamma will constrain models of Novae INTEGRAL

24 If total yield of 22 Na is understood, the carbonaceous meteoritic grains enriched in 22 Ne could be linked to nova sites. The isotopic abundance determined from such grains would provide further constraints on nova models. But, rate of 21 Na(p, γ) 22 Mg reaction unknown; Goal of E824

25 Levels of 22 Mg Proton capture on 21 Na dominated by isolated narrow resonances at T ~ 0.4 GK. Knowledge so far based on * transfer reactions, e.g. (p,t) * isospin mirror nucleus 22 Ne

26 21 Na Basic Experimental Approach 21 Na + p 22 Mg + γ Inverse kinematics H 2 Target γ θ 22 Mg Recoil Detector Advantage: θ < ~ 1 deg, could accept all recoils Challenges: Requires: Beam and recoil have ~same momentum. Rate of beam >>> rate of recoils (10 11 /1). Beam is radioactive leading to background. Intense source of radioactive 21 Na - ISAC Efficient detection of 22 Mg Very efficient rejection of 21 Na DRAGON Windowless hydrogen gas target

27 PROBLEMS: - Reaction governed by weak resonances - Requires intense 21 Na radioactive beam - Requires hydrogen gas target - Requires high beam suppression - Intense gamma background around 21 Na(p,γ) 22 Mg GOAL: WHY: HOW: Measure astrophysical rate at explosive stellar temperatures (Nova) Clarify mechanism of nova explosion Inverse kinematics using 21 Na beam

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29 The DRAGON Gas Target windowless, recirculating, differentially pumped inner cell: 11 cm, 4.5 Torr thickness: (3.65 +/- 0.12) at/cm 2

30 DRAGON Gamma Array 30 BGO scintillator units GEANT simulations Experimental verifications

31 Eye of the DRAGON

32 Gas Profile Measurement theory practice theory theory theory L eff =12.4±0.2 mm Replace reduces opening inner collimator holes by factor by mm Reduces opening holes by factor 22 Almost almost no no gas gas outside inner cell L eff (6/8) = B /B * L geo (1.5)

33 Measurement of Beam Energy Approach: -Calibrate NMR probe for MD1 -Use known narrow resonances 21 Ne(p,γ) at E cm = kev 20 Ne(p, γ) at E cm = kev 24 Mg (p, γ) at E cm = kev

34 Calibration Reactions Reaction E [kev] ωγ [ev] lit. Φ [mrad] ωγ [ev] 20 Ne(p,γ) / / Ne(p,γ) / / Ne(p,γ) / / Mg(p,γ) / / Mg(p,γ) / / Mg(p,γ) / /

35 Beam Suppression with DRAGON

36 Initial Results E cm = 821 kev Coincidence not needed Gamma Recoil.

37 Initial Results 21 Na(p,γ) 22 Mg at E cm = 821 kev ωγ = 556 +/-77 mev E = /- 1.9 kev Γ = /- 2.8 kev

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39 E beam = 220 kev/u E c.m. = 212 kev I( 21 Na) 2 x 10 9 s -1 BGO-DSSD coincidence Prompt γ recoil coin. BGO Efficiency

40 Results for 212 Resonance Thick target yield -only mid point used Resonance energy E cm = 205.7±.5 kev Not 212 kev Why? E lit = 214 kev Mass of 22 Mg = ±1.3 kev Not kev

41 Resonance Strength for MeV state Thick target yield; Y = 2 λ 2 M + m m ωγ de dx 1 ωγ = 1.03 ± 0.16 stat ±0.14 sys Accepted PhysRevLett March 5, 2003

42 Stellar Rate for 21 Na(p,γ) 22 Mg Reaction N A σν = 1.54 x (µt 9 ) -3/2 ωγ exp[ E R /T 9 ] Bateman et al Jose et al E824

43 Summary Report on E Na(p,γ) 22 Mg Received 21 Na beam ( 2 x 10 9 ;~600 epa) DRAGON operational -used DSSSD as focal plane detector -used beta activity,fc and elastics for flux -used BGO gamma despite high γ bgd. Measured ωγ, Γ for resonance at E cm =821 kev Measured ωγ for resonance at E cm = 212 kev Measured new mass excess for 22 Mg Preliminary results (ωγ) from other levels -E cm = 336 kev (no coincidences) -E cm = 461 kev (ωγ < 0.2 mev) -E cm = 545 kev (ωγ ~ 8 mev) -E cm = 747 kev (ωγ ~ 171 mev)

44 Scientific Collaborators - E824 Simon Fraser Univeristy Shawn Bishop John D Auria Mike Lamey Wenjie Liu Chris Wrede TRIUMF Lothar Buchmann Dave Hutcheon Alison Laird Art Olin Dave Ottewell Joel Rogers Colorado School of Mines Uwe Greife Cybele Jewett McMaster University Alan Chen University of Northern B.C. Dario Gigliotti Ahmed Hussein Saha Insitute of Nuclear Physics Mohan Chatterjee Yale University Peter Parker Rachel Lewis Ruhr-Universitat Bochum Sabine Engel Frank Strieder University of Tokyo Shigeru Kubono S. Mitimasa

45 Planned DRAGON Experiments Radioactive Beams 19 Ne(p,γ) 20 Na hot CNO breakout; rp process 13 N(p,γ) 14 O DC hot CNO breakout 17 F(p,γ) 18 Ne hot CNO breakout 25 Al(p,γ) 26 Si rp process; 26 Al production 15 O(α,γ) 19 Ne hot CNO breakout; x-ray burst 30 P(p,γ) 31 S nova mechanisms; rp process Stable Beams 12 C(α,, γ) 16 O 12 C( 12 C,, γ) 24 Mg approved experiments ISAC II Experiments 34 Ar(p,γ) 35 K rp process 56 Ni(p,γ) 57 Cu rp process needs CSB 57 Cu(p,γ) 58 Zn rp process

46 Planned/Proposed Experimental Facilities at ISAC (II) ISAC II March 7, 2003 ISAC II EXPERIMENTAL HALL From SE Entry Door Planned Facilities TIGRESS (8M CD) TITAN (3M CD) HERACLES BIG DRAGON TUDA II 123 x 90 x 33 h ft 2

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48 ISAC-II: Stage Device E in E out A/q V eff (MeV/u) (MeV/u) (MV) CSB RFQ IH-DTL SCDTL

49 ISAC-II: Stage Device E in E out A/q V eff (MeV/u) (MeV/u) (MV) CSB RFQ IH-DTL SCDTL

50 HERACLES TUDA-II BIG DRAGON TIGRESS

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52 Concluding Remarks ISAC (with ISAC II) is now a premier radioactive beams facility in the world Experimental program has started Many facilities now operational 21 Na(p,γ) 22 Mg has been measured in inverse kinematics using DRAGON

53 Concluding suggestions (RIA Workshop-OakRidge) Be clear about the objectives of the facility Bring team together with common goal Develop detailed specifications Ensure good communications between builders and scientists Maintain close contact with progress Long term support for university labs to develop techniques before RIA RIA needs multiple beam lines ISAC is a premier radioactive beams facility Available as site for tests and experiments