Collective modes: past, present and future perspectives · Osaka, Japan; 16-19 November 2015 7...
Transcript of Collective modes: past, present and future perspectives · Osaka, Japan; 16-19 November 2015 7...
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1Osaka, Japan; 16-19 November 2015
Collective modes: past, present and
future perspectives
Muhsin N. Harakeh
KVI, Groningen; GANIL, Caen
International Symposium on High-resolution
Spectroscopy and Tensor interactions (HST15)
Osaka, Japan
16-19 November 2015
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M. Itoh
L=0 L=1
L=2 L=3
ISGMR ISGDR
ISGQR ISGOR
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Microscopic structure of ISGMR & ISGDR
3ћω excitation (overtone of c.o.m. motion)
Transition operators:
OvertoneSpurious
c.o.m. motion
Constant Overtone
2ћω excitation
Microscopic picture: GRs are coherent (1p-1h) excitations
induced by single-particle operators
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DN = 2 E2 (ISGQR)
&
DN = 0 E0 (ISGMR)
DN = 1 E1 (IVGDR)
IVGDR
t rY1
ISGMR
r2Y0
ISGQR
r2Y2
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Equation of state (EOS) of nuclear matter
More complex than for infinite neutral liquids
Neutrons and protons with different interactions
Coulomb interaction of protons
1. Governs the collapse and explosion of giant stars
(supernovae)
2. Governs formation of neutron stars (mass, radius, crust)
3. Governs collisions of heavy ions.
4. Important ingredient in the study of nuclear properties.
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0
2
22 )/(
9
d
AEdKnm
E/A: binding energy per nucleon
ρ : nuclear density
ρ0 : nuclear density at saturation
For the equation of state of symmetric
nuclear matter at saturation nuclear
density:
and one can derive the incompressibility
of nuclear matter:
0)/(
0
d
AEd
J.P. Blaizot, Phys. Rep. 64, 171 (1980)
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Isoscalar Excitation Modes of NucleiHydrodynamic models/Giant Resonances
Coherent vibrations of nucleonic fluids in a nucleus.
Compression modes: ISGMR, ISGDR
In Constrained and Scaling Models:
F is the Fermi energy and the nucleus incompressibility:
KA =r2(d2(E/A)/dr2)r =R0
J.P. Blaizot, Phys. Rep. 64 (1980) 171
2
277 253
A F
ISGDR
KE
m r
+ ћ
2ISGMRAEr
K
m ћ
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Giant resonances
Macroscopic properties: Ex, G, %EWSR
Isoscalar giant resonances; compression
modes
ISGMR, ISGDR Incompressibility,
symmetry energy
KA = Kvol + Ksurf A1/3 + Ksym((NZ)/A)2+KCoulZ
2A4/3
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ISGQR, ISGMR
KVI (1977)
Large instrumental background
and nuclear continuum!
208Pb(,) at E=120 MeV
M. N. Harakeh et al., Phys. Rev. Lett. 38, 676 (1977)
10.9 MeV
13.9 MeV
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ISGMR, ISGDR
ISGQR, HEOR
100 % EWSR
At Ex= 14.5 MeV
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BBS@KVI
Grand Raiden@
RCNP
(,) at E~ 400
& 200 MeV at
RCNP & KVI,
respectively
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ISGQR at 10.9 MeV
ISGMR at 13.9 MeV
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0 ′ 3°
0 ′ 1.5°
1.5 ′ 3°
Difference
Difference of spectra
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Multipole decomposition analysis (MDA)
a. ISGR (L<15)+ IVGDR (through Coulomb excitation)
b. DWBA formalism; single folding transition potential
fraction EWSR :)(
section) cross(unit section crossDWBA :
.
),(
section cross alExperiment :
.exp
),(
.
),()(
.exp
),(
..
2
..
2
..
2
..
2
Ea
calc
L
EdEd
d
EdEd
d
calc
L
EdEd
dEaE
dEd
d
L
mc
mc
mc
L
Lmc
)'())'(|,'(|')(
])'(
))'(|,'(|)'())'(|,'(|)[,'('),(
00
0
00
rrrrVrdrU
r
rrrVrrrrVErrdErU LL
+
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Transition density
ISGMR Satchler, Nucl. Phys. A472 (1987) 215
ISGDR Harakeh & Dieperink, Phys. Rev. C23 (1981) 2329
Other modes Bohr-Mottelson (BM) model
)10)3/25(11(
6
)()]4(3
5103[
3),(
2224
222
1
02
2221
1
+++
rrr
R
mAE
rdr
d
dr
dr
dr
drr
dr
dr
REr
ErmA
rdr
drEr
+
2
22
0
000
2
)(]3[),(
21
222
2
222
0
2
)2(
)12()(
)(),(
+
+
L
L
LL
LL
r
r
mAEL
LLc
rdr
dEr
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18Osaka, Japan; 16-19 November 2015
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(,) spectra at 386
MeV
MDA results for L=0 and L=1
ISGDR ISGDR
ISGDR ISGDR
ISGMR
ISGMR
ISGMR
ISGMR
Uchida et al., Phys. Lett. B557 (2003) 12
Phys. Rev. C69 (2004) 051301116Sn
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E/A: binding energy per nucleon KA: incompressibility
ρ : nuclear density
ρ0 : nuclear density at saturation
KA is obtained from excitation
energy of ISGMR & ISGDR
KA =0.64Knm- 3.5
J.P. Blaizot, NPA591, 435 (1995)
208Pb
0
2
22 )/(
9
d
AEdKnm
Nuclear matter
In HF+RPA calculations,
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This number is consistent
with both ISGMR and ISGDR Data
and
with non-relativistic and relativistic calculations
From GMR data on 208Pb and 90Zr,
K = 240 10 MeV [ 20 MeV]
[See, e.g., G. Colò et al., Phys. Rev. C 70 (2004) 024307]
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Isoscalar GMR strength
distribution in Sn-isotopes
obtained by Multipole
Decomposition Analysis
of singles spectra
obtained in ASn(,)
measurements at
incident energy 400 MeV
and angles from 0º to 9º
T. Li et al., Phys. Rev. Lett. 99, 162503 (2007)
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KA ~ Kvol (1 + cA-1/3) + Kt ((N - Z)/A)2 + KCoul Z2A-4/3
KA - KCoul Z2A-4/3 ~ Kvol (1 + cA-1/3) + Kt ((N - Z)/A)2
~ Constant + Kt ((N - Z)/A)2
We use KCoul - 5.2 MeV (from Sagawa)
(N - Z)/A112Sn – 124Sn: 0.107 – 0.194
KA = Kvol + Ksurf A1/3 + Ksym((NZ)/A)2+Kcoul Z
2A4/3
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Kt 550 100 MeV
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MeV75555 tK
D. Patel et al., Phys. Lett. B 718, 447 (2012)
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RPA [K = 240 MeV]; RRPA FSUGold [K = 230 MeV];
RMF (DD-ME2) [K = 240 MeV]; (QTBA) (T5 Skyrme) [K = 202 MeV]
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RRPA: FSUGold [K = 230 MeV]; SLy5 [K = 230 MeV];
NL3 [K = 271 MeV]
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E. Khan, PRC 80, 011307(R) (2009)
The Giant Monopole Resonances in Pb isotopes
E. Khan, Phys. Rev. C 80, 057302 (2009).
Mutually Enhanced
Magicity (MEM)?
K = 230
K = 230
K = 216
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10 20 30 40
E (MeV)
0
2000
4000
6000
8000
Cou
nts
204Pb206Pb208Pb
0 spectra
x
0
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Conclusions!
There has been much progress in understanding
ISGMR & ISGDR macroscopic properties
Systematics: Ex, G, %EWSR
Knm 240 MeV
Kt 500 MeV
Sn and Cd nuclei are softer than 208Pb and 90Zr.
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Challenges with exotic beams
• Inverse kinematics
56Ni(α,α)56Ni*
α = Target56Ni = Projectile
• Intensity of exotic beams is very low (104 – 105 pps)
• To get reasonable yields thick target is needed
• Very low energy ( sub MeV) recoil particle will not come out
of the thick target
Ex = 0 MeV
2o 4o 6o8o
Ex = 30 MeV
Ex = 20 MeV
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Nuclear structure studies with
reactions in inverse kinematics
4He target
heavy projectile heavy ejectile
recoiling
(,)
- Possible at FAIR, RIKEN, GANIL, FRIB(beam energies of 50-100 MeV/u are needed!)
Approach at GSI-FAIR (EXL):
Helium gas-jet targetMeasure the recoiling alphas
Inconvenience:
difficulty to detect the low-energy alphas
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EPJ Web of Conferences 66, 03093 (2014)
Experimental storage ring at GSI
Luminosity: 1026 – 1027 cm-2s-1
Storage Ring
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Detection system @ FAIR
EXL recoil prototype detector has been commissioned
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Active target
A gas detector where the target gas also acts as a detector
Good angular coverage
Effective target thickness can be increased without
much loss of resolution
Detection of very low energy recoil particle is possible
MAYA active-target detector at GANIL
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Basics of kinematics reconstruction inside MAYA
Timing information from Amplification wires
Range → Energy
(SRIM)
R2d → R3d , θ2d → θ3d
500 mbar
95% He and 5% CF4
20 Si detectors
80 CsI detectors
Beam 56Ni
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3rd dimension from timing information of the anode wires
Range Energy
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Kinematics plot
56Ni(α,α)56Ni*
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Peak fitting method
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Participants
M. Csatlós
L. Csige
J. Gulyás
A. Krasznahorkay
D. Sohler
ATOMKI
A.M. van den Berg
M.N. Harakeh
M. Hunyadi (Atomki)
M.A. de Huu
H.J. Wörtche
KVI
U. Garg
T. Li
B.K. Nayak
M. Hedden
M. Koss
D. Patel
S. Zhu
NDU
H. Akimune
H. Fujimura
M. Fujiwara
K. Hara
H. Hashimoto
M. Itoh
T. Murakami
K. Nakanishi
S. Okumura
H. Sakaguchi
H. Takeda
M. Uchida
Y. Yasuda
M. Yosoi
RCNP
C. Bäumer
B.C. Junk
S. Rakers
WWU
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E605: ISGDR in 56Ni EXL Collaboration
Soumya Bagchi Juan Carlos Zamora
Marine Vandebrouck
M. Vandebrouck et al., Phys. Rev. Lett. 113 (2014) 032504
M. Vandebrouck et al., Phys. Rev. C 92 (2015) 024316
S. Bagchi et al., Phys. Lett. B751 (2015) 371
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Thank you for your attention
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45Osaka, Japan; 16-19 November 2015
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46Osaka, Japan; 16-19 November 2015
Kt = -500 +125 MeV100
M. Centelles et al., Phys. Rev. Lett. 102, 122502 (2009)
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47Osaka, Japan; 16-19 November 2015
M.N. Harakeh et al., Nucl. Phys. A327, 373 (1979)
10.9 MeV
13.9 MeV
11.0 MeV
14.0 MeV
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48Osaka, Japan; 16-19 November 2015
S. Brandenburg et al., Nucl. Phys. A466 (1987) 29
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49Osaka, Japan; 16-19 November 2015
S. Brandenburg et al.,
Nucl. Phys. A466 (1987) 29
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50Osaka, Japan; 16-19 November 2015
S. Brandenburg et al., Nucl. Phys. A466 (1987) 29
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51Osaka, Japan; 16-19 November 2015
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52Osaka, Japan; 16-19 November 2015
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53Osaka, Japan; 16-19 November 2015
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54Osaka, Japan; 16-19 November 2015
Excitation energy of 56Ni
Data (Not efficiency corrected) Data (Efficiency corrected)
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55Osaka, Japan; 16-19 November 2015
Peak fitting method Background shape fixed manually (Background 1)
Total fit = 9 Gaussian
Func. + PoL4 + CFinal background
(PoL4 + C)
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56Osaka, Japan; 16-19 November 2015
E* = 33.5 MeV, L = 1
E* = 22.5 MeV, L = 1
E* = 14.5 MeV, L = 2
E* = 28.5 MeV, L = 1E* = 25.5 MeV, L = 1
E* = 17.5 MeV, L = 1 E* = 19.5 MeV, L = 0
E* = 11.5 MeV, L = 2E* = 8.5 MeV, L = 1d
σ/d𝜴
[mb
/sr]
θCM [deg]Background 1
Background 2