physics loi for neda
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Physics LOI for NEDA. R. Wadsworth University of York , G. de Angelis INFN LNL. Istanbul 19 june 2009. Defining the Physics. Nuclear Astrophysics Element abundances in the Inhomogeneous Bib Bang Model (Weizmann, Soreq, GANIL, York collaboration) - PowerPoint PPT PresentationTRANSCRIPT
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Physics LOI for NEDA
Istanbul 19 june 2009
R. Wadsworth University of York , G. de Angelis INFN LNL
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Defining the Physics• Nuclear Astrophysics
– Element abundances in the Inhomogeneous Bib Bang Model (Weizmann, Soreq, GANIL, York collaboration)
– Isospin effects on the symmetry energy and stellar collaps
• Nuclear Reactions– Level densities of neutron rich nuclei (Naples,
Bordeaux, Debrecen, LNL, Florence collaboration)– Fission dynamics of neutron-rich intermediate fissility
systems• Nuclear Structure
– Probe of the T=0 correlations in N=Z nuclei: The structure of 92Pd
– Coulomb Energy Differences in isobaric multiplets: T=0 versus T=1 states
– Coulomb Energy Differences and Nuclear Shapes– Low-lying collective modes in proton rich nuclei
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rapid proton capture,
Reaction Paths in Nuclear Astrophysics
Nuclear Astrophysics : Element abundances in the Inhomogeneous Bib Bang Model
(Weizmann, Soreq, GANIL, York collaboration)
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Letter of Intent for the proposed “Neutron Wall” at SPIRAL-II
Measurement of the 8Li(,n) 11B ReactionMichael Hass
for theWeizmann-Soreq-GANIL-York collaboration
We propose to study the 4He(8Li,n)11B reaction using 8Li beams at SPIRAL-II. The R&D efforts to produce unsurpassed intense beams of 8Li at SPIRAL-II may result in 8Li very well becoming one of the first radioactive beams to be used at SPIRAL-II. This fact, together with the unique performance of the proposed neutron wall and of other ancillary charge-particle detectors will provide an ideal experimental setup for such studies. The data thus obtained should clarify the poorly known cross section for this reaction, which is important for several scenarios in the field of explosive nucleo-synthesis.
Michael Hass - 8Li(,n)11B
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Fig. 1 Experimental data available in the literature
Fig. 2 States in 12B that are in the region of interest for cosmological (and stellar) environment(s) at temperatures of ~ 1 GK
Michael Hass - 8Li(,n)11B
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Expected Yields for a BeO target:SARAF (40 MeV, 2 mA): 8∙1012
[6He/sec]SPIRAL2 (40 MeV, 5 mA): 2∙1013
[6He/sec]
Expected Yields for a BN target:SARAF (40 MeV, 2 mA): 2∙1012
[8Li/sec]
SPIRAL2 (40 MeV, 5 mA): 5∙1012 [8Li/sec]Michael Hass - 8Li(,n)11B
11B
Under current R&D:
• Diffusion and effusion in the material• Ionization and extraction• Choice of ion source
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Fig. 3 The proposed experimental setup.
Issues for consideration
• 8Li@SPIRALII The present scheme uses the 11B(n,a)8Li reaction with secondary neutrons from the initial 5 mA, 40 MeV d beam with a porous BN target. Post-acceleration. Energy degrader.
• The neutron wall
• Charge particle (11B) detection
Michael Hass - 8Li(,n)11B
Neutron (energy) + charge particle detections
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Why is it important to study the symmetry energy ?
Esym=bsym(T)(N-Z)2/A
• As a part of the nuclear Equation Of State it may influence the mechanism of Supernova explosion
• General theoretical agreement on its temperature dependence (LRT+QRPA vs. large scale SMMC)
• Possible consequences of T dependence of Esym on core-collapse Supernova events
• Effects enhanced by the instrinsic isospin dependence of Esym
Fusion-evaporation reactions: Esym affects the particle B.E.
(Naples, Debrecen, LNL, Florence collaboration)
Isospin effects on the symmetry energy and stellar collaps
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SYMMETRY ENERGY
m(T) 0 < T < 3 MeV - 98Mo, 64Zn, 64Ni
-LRT – QRPA
Decrease of the effective mass Increase of Esym
Esym(T)= bsym(T) x (N-Z)2/A
bsym(T)=bsym(0)+(h2ko2m/6mk)[m(T)-1 – m(0)-1]
m(T)=m + [m(0) – m]exp(-T/To)
Framework: Dynamical ShellModel
Hartree-Fock Coupling single particle statesto suface vibrations
Nucleon effective mass
m
mmm k
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Isospin effects on the symmetry energyStudy with RIB’s from SPIRAL2
The isospin effects are larger than those due to the change of level density parametera from A/8 to A/10. A strong sensitivity on isospin is also expected for the ER yields. (Same observables and experimental setup)
109Mo Ex=16 MeV1n channel
105Zr + 4He 109Mo
Neutron energy and multiplicity information + Charged particle information + gamma ray information
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Nuclear Reaction Mechanisms:
Evaporative neutron emission as a probe for the level density of hot neutron-rich compound nuclei (Naples, Bordeaux, Debrecen, LNL, Florence collaboration)
Neutron energy and multiplicity information + Charged particle information + gamma ray information
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Why is it important to study the level density ?
Level density is a basic ingredient for x-section calculations
Astrophysical processes “Astrophysical Reaction Rates from Statistical Model Calculations”, ADNDT 75 (2000) 1-351
SHE’s production
Capture of two nuclei in the attractive potential pocket.
ER capture PCN Psurv
Survival probability against fission.
Probability of forming a compact compound nucleus (CN).
Evaporative process: Statistical Model
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Isospin effects on the level density parameter a
20<A<110 ENSDF
Form A:
Form B:
Form C:
Form C provides the best reproduction ofexperimental leveldensities
Strong reduction
of level density
for exotic nuclei
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0 1 2 3 4 5 6
100
101
102
103
Co
un
ts
En,cm(MeV)
Standard N-Z Z-Zo
0 1 2 3 4 5 6
100
101
102
103
Co
un
ts
En,cm (MeV)
Standard N-Z Z-Zo
Isospin effects on the level density parameter aStudy with RIB’s from SPIRAL2
A strong sensitivity on isospin is also expected for the evaporation residue yields
Experimental setup: NEDA coupled to the gamma ray spectrometers EXOGAMor AGATA and/or the spectrometer VAMOS. (NEDA: TOF Measurements 3% resolution, energy threshold 1 MeV). Lcp could be also measured by Diamant.
84Ge + 4He
134Sn + 4He
n
n
Observables
- xn channels)
- n en. spectra
- ER yields
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Fission dynamics of neutron-rich intermediate fissility systems (under study)
Open questions in fission dynamics: Fission delay, nature of dissipation (one or two body) and its dependence on temperature and nuclear deformation
Systems of intermediate fissility (A 150): possibility to measure observables in both fission and evaporation residue channels
Fission BarrierBf (L=50 )
(MeV)
n- Prescissionmultiplicity
Mn
Fission time <Tfiss>
(10-21 s)
124Ce 16.3 0.046 61
144Ce 29.7 2.1 103
Measurements on nuclei with the same Z and different isospin allow to Study of the role of isospin in fission dynamics:
230 MeV 32S + 92Mo Lcrit = 74 750 MeV 118Pd + 26Mg Lcrit = 81 Ex122 MeV
Preliminary results from a dynamical model based on three dimensional Langevin equations
Experimental setup: NEDA coupled to fission fragment detectors
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Nuclear Structure : N=Z nuclei
Probe of the T=0 correlations in N=Z nuclei: The structure of 92Pd
Coulomb Energy Differences in isobaric multiplets: T=0 versus T=1 states
Coulomb Energy Differences and Nuclear Shapes
Low-lying collective modes in proton rich nuclei
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Probe of the T=0 correlations in N=Z nuclei: The structure of 92Pd
(LNL, Stockholm, York collaboration)
Neutron multiplicity information + charged particle + gamma ray information
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56Ni (108pps) + 40Ca 92Pd (1 mb), 94Ag (1 mb)
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Coulomb Energy differences in isobaric multiplets: T=0 versus T=1 states
(Sofia, Padova, York, Ganil, LNL collaboration)
Neutron multiplicity ( and energy) information +Charged particle + gamma ray informations
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Example: Electromagnetic Transition Probabilities
If Isospin Symmetry is valid:
E1 (T=0) transitions in N=Z nuclei are forbidden
E1 transition in mirror pairs have identical strength(higher sensitivity due to interference)
Crucial Probe of the isospin symmetry and of its validity with increasing A and Z
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Observation of a forbidden E1 transition in 64Ge
64 32 32
64Ge
EUROBALL IV + Plunger experiment
E. Farnea et al. Phys. Lett. 551B, 56 (2003)
forbidden E1?
32S+40Ca 125 MeV
Electromagnetic Transition Probabilities
Dobaczewski and HamamotoPhys. Lett. B345 181 (1995)
Dobaczewski and HamamotoPhys. Lett. B345 181 (1995)
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Isospin mixing via the IVGMR provides an induced isoscalar component
In mirror T=0 transitions• Isovector terms have opposite sign • Isoscalar terms have equal sign
B(E1) = BIS(E1) – BIV(E1)
J. Ekman et al. PRL 92, 132502 (2004)
B(E1) strengths are identical in T=1/2 mirror pairs
B(E1) = BIS(E1) + BIV(E1)
Isospin Mixing in Mirror Pairs
In the validity of isospin symmetry
1) Charge invariance of the nuclear interaction
2) Long-wavelength approximation
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67Se 67As
Electronic timing measurements
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N=Z nuclei: Reactions with RIBS
• 34Ar + 40Ca (105-120 MeV)– 69Br + p 1 mb – 71Kr + 2pn 5 mb– 68Br + pn 0.2 mb– 72Rb + pn 0.1 mb– How do we study the proton unbound cases e.g. 68,69Br?
• 58Cu + 28Si (~200 MeV)– 81Nb + n 0.1 mb
• 56Ni + 28Si (~200MeV) – 79Zr + n 0.2 mb
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Coulomb Energy Differences and Nuclear Shapes
(York, LNL, Padova, Sofia collaboration)
Neutron multiplicity information, charged particle and gamma information
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N=Z nuclei: Reactions with RIBS
• 34Ar, 30S + 40Ca (105-120 MeV)– 69Br, 65As + p 1 mb – 71Kr, 67Se + 2pn 5 mb– 68Br, 64As + pn 0.2 mb– 72Rb, 68Br + pn 0.1 mb– How do we study the proton unbound cases e.g. 68,69Br?
• 58Cu + 28Si (~200 MeV)– 81Nb + n 0.1 mb
• 56Ni + 28Si (~200MeV) – 79Zr + n 0.2 mb
A=64, 68 T=1 triplet
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Nuclear Structure :Low-lying collective modes in proton rich nuclei
Valencia, INFN LNL , Paris, INFN MI collaboration.
Neutron multiplicity (and energy), charged particle and High energy gamma information
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34Ar + 16O 44Cr + 2n
34Ar 108 pps
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Dipole Excitations towards the Proton Drip-Line
CENTROID ENERGY OF THE LOW-LYING STRENGTH
CENTROID ENERGY OF THE LOW-LYING STRENGTH
LOW-LYING TRANSITION STRENGTH B(E1)
LOW-LYING TRANSITION STRENGTH B(E1)
PROTON PYGMY DIPOLE RESONANCE
PROTON PYGMY DIPOLE RESONANCE
Paar, Vretenar, Ring, Phys. Rev. Lett. 94, 182501 (2005)
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Dipole Excitations towards the Proton Drip-Line
CENTROID ENERGY OF THE LOW-LYING STRENGTH
CENTROID ENERGY OF THE LOW-LYING STRENGTH
LOW-LYING TRANSITION STRENGTH B(E1)
LOW-LYING TRANSITION STRENGTH B(E1)
PROTON PYGMY DIPOLE RESONANCE
PROTON PYGMY DIPOLE RESONANCE
Paar, Vretenar, Ring, Phys. Rev. Lett. 94, 182501 (2005)
24Mg(p,p2n) 22Mg
22Mg + 16O 32Ar + 2n 22Mg 108 pps
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Thanks for attention
• Present LOIs still under development
• Please join LOIs or present new ones
• Upgrading of the physics case is on the way
• Definition of the “day one” experiments