THE ACCULINNA AND ACCULINNA-2 RADIOACTIVE ION BEAM FACILITY AT DUBNA: STATUS AND PERSPECTIVES
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1 THE ACCULINNA AND ACCULINNA-2 RADIOACTIVE ION BEAM FACILITY AT DUBNA: STATUS AND PERSPECTIVES Grzegorz Kamiński for the ACCULINNA group FLNR, JINR, DUBNA International Nuclear Physics Conference (INPC2016) Adelaide Convention Centre, Australia September 11-16,
2 Short outline Introduction: Light RIB facility at FLNR: ACCULINNA Status of the ACCULINNA-2 project first day experiments at ACCULINNA-2 2
3 Superheavy and superlight research at FLNR, JINR Elements synthesized at FLNR Elements: (IUPAC approval) 113 Nihonium (2016) 114 Flerovium (2011) 115 Moscovium (2016) 116 Livermorium (2011) 117 Tennessine (2016) 118 Oganesson (2016) Last two decades: Elements synthesized at FLNR Superheavy 3
4 Superheavy and superlight research at FLNR, JINR Elements synthesized at FLNR Elements: (IUPAC approval) 113 Nihonium (2016) 114 Flerovium (2011) 115 Moscovium (2016) 116 Livermorium (2011) 117 Tennessine (2016) 118 Oganesson (2016) Last two decades: Elements synthesized at FLNR Superheavy ACCULINNA&ACCULINNA-2 Recent achievements Current developments Future proepscts Light & Superlihght 4
5 ACCULINNA-2 in perspective 5
6 Energy MeV/nucleon Beams and ACCULINNA-2 somewhere among other facilities Atomic number 6
7 RIBs from ACCULINNA-2 Primary beam Radioactive Ion Beam Ion Energy, MeV/u Ion Energy, MeV/u Intensity, s 1 (per 1 pµa) Purity, % 11 B 32 8 He 26 3* N Li 37 3* B Be 26 1* N Be * O Be 35 2* Ne 44 calculations done with LISE++ 17 C 33 3* C 35 4* S O 40 2*10 2 (U400M upgrade) 10 B 39 7 Be 26 8* Ne Ne 34 2* S Be 31 2* (with RF kicker) (with RF kicker)
8 Z Scope of activity for ACCULINNA-2 27 S 4 H 9 He 10 He ACC ACC2 - first experiments ACC2 - further studies 8
9 Competitive light nuclei RIB program at ACCULINNA-2 Energy range and reaction selection Intermediate energy reactions (20-70 MeV/nucleon) High energy reactions (> MeV/nucleon) Transfer reactions Knockout reactions Population of highly aligned states in the intermediate energy transfer reactions Prospects for specific correlation studies Complementary information from different reaction mechanism Lower reaction energy - easier to get higher energy resolution Correlations and few-body dynamics studies Correlations for aligned states populated in the direct reactions Few-body dynamics near the driplines Correlations in the three-body decays: two extra degrees of freedom 9
10 ACCULINNA-2 instrumentation development Instrumentation development Tritium target system for ACC-2 Zero-angle spectrometer (2016) Velocity filter (RF-kicker) (2017) Cryogenic tritium target cell Detectors development High-resolution telescope array Neutron detection system (stilbene crystals) γ-array GADAST New Optical Time Projection Chamber OTPC (UW, Warsaw) 10
11 Layout of ACCULINNA-2 11
12 Layout of ACCULINNA-2 ACC-2 RIPS FLNR JINR RIKEN Ω [msr] p/p [%] ±3.0 ±3.0 Rp/ p Bρ [Tm] Length [m] E [AMeV] Additional RF-kicker RF-kicker RIB Filter 12 RIPS layout from T. Kubo / Nucl. Instr. and Meth. in Phys. Res. B 204 (2003)
![Layout of ACCULINNA-2 ACC-2 RIPS FLNR JINR RIKEN Ω [msr] 5.](/docs-images/72/67060036/images/13-0.jpg "8 5 p/p [%] ±3.0 ±3.0 Rp/ p 2000 1500 Bρ [Tm] 3.9 5.")
![76 Length [m] 38 27 E [AMeV] 6 60 50 90 Additional RF-kicker RF-kicker](/docs-images/72/67060036/images/13-1.jpg "RIB Filter 13 RIPS layout from T. Kubo / Nucl. Instr. and Meth.")
13 Layout of ACCULINNA-2 ACC-2 RIPS FLNR JINR RIKEN Ω [msr] p/p [%] ±3.0 ±3.0 Rp/ p Bρ [Tm] Length [m] E [AMeV] Additional RF-kicker RF-kicker RIB Filter 13 RIPS layout from T. Kubo / Nucl. Instr. and Meth. in Phys. Res. B 204 (2003)
14 From contract with SIGMA PHI to installation:
15 Layout of ACCULINNA «In the beginning, there was Chaos» Greek Mythology The Creation
16 Area & floor preparation 1 st delivery January
17 Installation Stands September
18 Installation & Alignment, Available magnets September
19 Installation & Alignment, all magnets and vacuum January
20 Magnets: some big ones 20
21 PS installation, full cabling and cooling July Support for shielding walls is prepared 21
22 Installation out of reach of the crane January
23 Room 2 23
24 Room 2: floor reinforcement ~11 tons ~9.1 tons Max deviation 0.9 mm 24
25 Room 2: Floor reinforcement Febr March Building structure pillars March March
26
27 The zero angle spectrometer : Full commissioning + Beam 2016: Zero-angle spectrometer 2017: RF kicker at F3 2017: New detectors : Tritium target at F : Cyclotron upgrade E HI : 60 to 80 AMeV 2 < Z HI < 36 I: 2 to 3 pµa SC ECR source 24 GHz vs 18 GHz better emittance : electrostatic vs stripping extraction
28 The near future Yoke 12.2 tons Coils 3 tons PARAMETERS values Maximum field - Bmax 1.382T Nominal field - Bnom 1.207T Minimum field - Bmin 0.403T Gap 180 mm Effective length for Bnom mm Effective length variation Bnom - Bmin 5.56mm nominal integrated field Blnom T.mm Ampere turns per pole for Bnom 93540A.t Ampere turns per pole for Bmin 29376A.t Ampere turns per pole for Bmax A.t Stored Energy for Bmax 99500J Good field region dimensions H ±250mm V ±65mm (info) Transverse Field Bnom 0/2.7x10-3 Midplane Transverse Field Bmin 0/2.2x 10-3 Midplane Integrated Field Bnom -1.53x10-3 /1.22x10-3 Integrated Field Bmin -1.39x10-3 /1.06x10-3
29 The zero angle spectrometer Multi-wire proportional chamber (MWPC) Protons, deuterons, tritons Bρ = 0.4 ~ 1.0 Tm Cone 0 ~ 14 Bρ=1.0 Bρ=0.4 RIB ±14 ±6 Bρ=1.1 Bρ=1.7 Heavy decay products Bρ = 1.1 ~ 1.7 Tm Cone 0 ~ 6 Neutrons (stilbene array) Distance to target > 2 m TOF accuracy < 1% 29
30 RF-Kicker Frequency range (MHz) 14,5-20 Peak voltage (KV) 120 GAP (mm) 70 Width of electrode (mm) Length of electrodes (mm) 700 Cylinder diameter (mm) Stem diameter (mm) Length of coaxial line from beam axis (mm) 120 min 1200 max 120 max 1830 RF power (Watts) Reactance Q
31 ACCULINNA&ACCULINNA-2 More details about proposed reactions at ACCULINNA-2 G. Kamiński talk, Thursday R3 : 16:05 31
32 7 H: experiments to be done at ACCULINNA-2 M.S. Golovkov et al., Phys. Lett. B 588, 163 (2004) Limit T 1/2 < 1 ns was set for the 7 H lifetime, which allowed the authors to estimate a lower limit of kev for the 7 H energy above the 3 H + 4n breakup threshold. L. V. Grigorenko et al., Phys. Rev. C 84, (R) (2011). Г, MeV T 1/2, s E T, MeV 8 He( 2 H, 3 He) 7 H 11 Li( 2 H, 6 Li) 7 H Missing mass spectrum Counts in 0 + state 2 x 10 2 dσ/dω 10 µb/sr 3 x 10 3 dσ/dω 10 µb/sr Resolution 400 kev 200 kev Exciting option is to try the 8 He + 3 H reaction. The 4n transfer can be searched for down to a limit of dσ/dω 10 nb/sr. The 2n transfer and triton transfer channels, as well as elastic scattering, will be accessible for study. 32
33 ACCULINNA-2 9 He from the 8 He( 2 H,p) 9 He reaction ACCULINNA ACCULINNA-2 Missing mass Counts Resolution 800 kev 300 kev θ 8He 12 o 0.3 o Combined mass Counts 3 x 10 4 Resolution kev A setup for the 9 He and 10 He study at ACCULINNA-2 Zero degree spectrometer
34 10 He: prospects assumed for ACCULINNA-2 S. I. Sidorchuk et al., Phys. Rev. Lett. 108, (2012) 10 He from 8 He( 3 H,p) 10 He Other reactions 10 He missing mass spectrum. Points with error bars correspond to the total data array; the grey histogram was obtained for ε < 5. The dashed histogram describes the behavior of the detection efficiency for 8Не-р coincidences ACCULINNA ACCULINNA-2 Missing mass spectrum Count number in 0 + state ~120 2 x 10 4 Resolution 500 kev 200 kev Resolution in θ 8He 12 o 0.3 o Correlation analysis for the tripple (p- 8 He-n) events Counts (E T = 0 10 MeV) 3 x Li( 2 H, 3 He) 10 He 14 Be( 2 H, 6 Li) 10 He Missing mass spectrum Counts in 0 + state 2 x x 10 3 Resolution 400 kev 200 kev 34
35 17 Ne Nuclear structure Nuclear astrophysics Combined mass approach to the study of decay modes of exotic nuclei. 17 Ne is 2p-halo candidate 17 Ne is only one known nuclear system, which excited state can decay through direct 2p emission. 2p radiative capture is a possible by-pass of the 15 O waiting point in the astrophysical rp-process Combined mass spectrum of 17 Ne measured by the Acculinna provided a limit Γ 2p / Γ γ < 8 * 10 5 [ P. Sharov et al., talk given at EXON2016 ]. Our task is to come to a level of Γ 2p / Γ γ ~ (2-3) * 10 6 in a priority experiment which will be carried out at ACCULINNA-2. proton telescope Beam 18 Ne Experimental setup. Γ 2p / Γ γ ratio measurment Target liquid hydrogen aluminum shield 35
36 β - delayed particle emission (example: 27 S) New decay channels possible Already known decay branches G. Canchel et al., Eur. Phys. J. A 12, 377 (2001). T 1/2 ( 27 S) = 15.5 ms; P(βp) = 2.3 ± 0.9%; P(β2p) = 1.1 ±0.5% 36
37 β - delayed particle emission (example: 27 S) New decay channels possible Specific equipment development: Warsaw Optical Time Projection Chamber (OTPC) Already known decay branches G. Canchel et al., Eur. Phys. J. A 12, 377 (2001). T 1/2 ( 27 S) = 15.5 ms; P(βp) = 2.3 ± 0.9%; P(β2p) = 1.1 ±0.5% K. Miernik et al., NIM A581(2007)194 No events with 3p emission observed (low statistics), but new results (new branching) for low energy (~300 kev) protons are expected. L. Janiak, UW, Warsaw p 27 S p p 27 S In 2017 a new measurment of β - delayed particle emission from 27 ACCULINNA-2 is planned much better statistic of two order of magnitude expected = hunting for 3p decay
38 Conclusions Glorious history of light exotic nuclei studies at JINR World-class current research program light exotic nuclei Specific energy range intermediate energy direct transfer reactions Specific techniques + theory school (few-body) correlation studies Clear plans for the nearest years: ACCULINNA-2 beam test this year Instrumentation development + accelerator upgrade = user facility 38
39 We plane to extend our studies on more exotic species THANK YOU FOR ATTENTION! 39
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