1 JINR: Current activities and Prospects Nuclear Engineering, Femto - and

is devoted to the

60th anniversary of Joint Institute for

Nuclear Research, Dubna

June 29 – July 3, 2015, Peterhof, Saint-Petersburg

26 March 1956 in Moscow
JINR – a Centre of Broad

International Partnership on the Russian Land

- 18 Member States
- 6 Associated Members States
about 700 research partners in
60 countries
- staff members ~ 5500

Programme: ‘2003 – 2009’ (complete and successful realization)

‘2010 – 2016’ (final draft approved by the Scientific Council, Sept. 2009 and CPP, Nov. 2009)
Road Map (2006-2017)

High Energy Physics
Nuclear Physics
Condensed Matter Physics

Basic Scientific Directions

Fundamental
Science

I.

DRIBs (I,II,III) –
Dubna Radioactive
Ion Beams
For the last

decade JINR has become one of the leading scientific centres in the world in low energy heavy-ion physics.

U400 and U400M isochronous cyclotrons are combined into the accelerator complex – project DRIBs which deals with the production of beams of exotic light neutron-deficient and neutron-rich nuclei in reactions with light ions.

Number of observed decay chains
Element 118 3
Element 116 26
Element 115 4
Element 114 43
Element 113 2
Element 112 8

U400)
Creation of the new experimental hall (≈ 2600м2)
Development

and creation of next generation set-ups
Creation of high current heavy ion accelerator DC200
(A≤ 100, E ≤ 10 MeV ·A, I≥10 pµA)

JINR’s Large-Scale Basic Facilities

DC200: MAIN PARAMETERS

is included in the

20-year European strategic programme of neutron scattering research.

Parameters

Fundamental and applied research in condensed matter physics and related fields –– biology, medicine, material sciences, geophysics, engineer diagnostics — aimed at probing the structure and properties of nanosystems, new materials, and biological objects, and at developing new electronic, bio- and information nanotechnologies.

from NEMO 3 to Super NEMO
2011 – First Module on-site

of NEMO 3
2012 – 2016 – Installation and data taking at Super Nemo

Expected Limits: T1/2(bb0n) > (1-2) x 1026 y, < 0.06 - 0.10 eV

Present Limits (90% CL) :
T1/2(0nbb) > 5.8 x 1023 y,
< 0.8 – 1.3 eV

Neutrino and Rare Phenomena Physics

From NOMAD to OPERA

OPERA: 2008 – 2009: start of data taking in full configuration
2010 – 2016: further data taking and analysis

1. JINR - Moscow 20Gbps telecommunication channel was put

into operation.
2. Increase of the JINR Central Information and Computing Complex performance up to 2400 kSI2K and the disk storage capacity up to 500 TB.

At present, JINR site is one of the 10 best sites of the worldwide Grid infrastructure (WLCG).

are trained at the UC
A vitally important task is attracting

of young people from
all the Member States to science

JINR is a school of excellence for the Member States!

MSU

MIPT

MEPI

Chairs:

MIREA

others

JINR UNIVERSITY CENTRE

“Dubna” International University

The UC offers graduate programmes in the fields of:
Elementary Particle Physics
Nuclear Physics
Theoretical Physics
Condensed Matter Physics
Technical Physics
Radiobiology

DIAS - TH

Dubna International
Advanced School
on Theoretical Physics

-200928 June – 13 July 2009
Organizing - informative forum
“Establishment

of the International Innovation Nanotechnology Centre in Dubna”.
1 – 2 July 2009

Large International Nanotechnology forums at JINR

technology has been developed to produce nuclear membranes by using

unique multicharged ion cyclotrons.
On the basis of this technology the nuclear membranes can be produced from various polymeric films.  

Scheme of nuclear
membrane manufacture

человеческий волос и микропоры трековой мембраны

а)

b)

c)

d)

e)

f)

Nanostructures of various modifications

complex of hadron therapy
Radiation Medicine

of scientific
schools.


Large and unique park of
basic facilities for

fundamental and
applied research.



Status of an international
intergovernmental organization.

Exotism of Nuclei

Introduction
Nuclear matter exotism

Hot nuclei
Super deformed

nuclei
Super dense nuclei
Neutron and proton nuclei
Super heavy nuclei

Borders of nuclear stability

Super neutron – rich nuclei of light elements (10He)
Nuclei close to N=20, 28 (28O, 40Mg)
Super heavy nuclei

Beams of accelerated exotic nuclei

matter
N-Z A
gas
T
hot fluid
High temperature matter
mixed phase
Isospin
density
Exotic Nuclei

a nucleus can endure
and finally survive….

and Interactions
Sp=0
Sn=0
Physics with Exotic Nuclei
New Decay Modes
2

p and n radioactivity

extreme test of models (shell model, shell model in continuum,

“ab initio”, cluster, etc)

9He

10He

Borromean nuclei
core+n+n – bound core+n n+n - unbound

(binary reactions)

A (a,b)B

MA+Ma= Mb+MB+Q/c2
Ра=Рь+Pв; Pa=O

Pb=PAMbcosΘ/(MA+Ma)+{2MbMB[EAMa/ (MA+Ma)+Q-E*]/
/(Mb+MB) -[PAMbsinΘ/(MA+Ma)]2}1/2

Mb Pb are measured → Q,E* are calculated →MB is obtained

middle
Еfficiency of neutron registration.
2 germanium detectors (maximum efficiency

of gamma registration)
1 beta detector

NEUTRON DETECTOR “TETRA” FOR TETRANEUTRON SEARCH

6Н

ER = 2.6  0.5 МэВ
Penionzhkevich et

all

ER = 3.5(5) МэВ
(ER  5.3 МэВ)

6Н  3Н+n+n+n , Г = 1.3  0.5 МэВ
Ter-Akopyan et all

nuclei properties

At. Data
Nucl. Tables 59 185 1995)
Mass

Formula Koura et al RIKEN-AF-NP-394

Predictions disagree
with each other

The variation of the shell gap and deformation as a function of N and Z could be a major challenger. A particular feature in this region is the progressive development of deformation in spite of the expected effect of spherical stability due to magicity of N=20 and N=28 shells.

et al Phys.(London) G28, L41 (2002)
M.Notani et al
Phys.Lett.

542B, 49 (2002)

Experimentally established:
The last particle bound Nitrogen isotope in 23N (N=16), Oxygen isotope is 24O( N=16)
The neutron drip line extends beyond N=20 and reaches N=24 for 34Ne and even N=26 for 37 Na isotopes.

strength of N=20 and N=28 shells is variable in the

region from carbon up to neon.

Appearance of new
magic numberN=16?

A particular feature in this region is the progressive development of
prolate deformation in spite of the expected effect of spherical stability due to the magicity of the neutron numbers N=20 and 28.
It was argued that the deformation may lead to enhanced binding energies in some of yet undiscovered neutron-rich nuclei.

for magnesium isotopes

37Na and 40Mg are defined the cliff of the neutron

drip line
Experimental evidence of progressive development of deformation in
spite of the expected effect of spherical stability due to magicity of N=20 and N=28 shells
New magic numbers (N=16 and N=26?) are appeared far from stability instead of N=20 and N=28
There are difficulties in the theoretical predictions of the neutron-drip line
Qualitative difference for Neutron Drip line Nuclei:

Shell model

around the Vanishing of the magic numbers
valley of stability far from stability ?

Shell closures far from stability :
N=20 : "Island of inversion" for neutron-rich nuclei (ex. 32Mg)
N=28 : Short Lifetime of the 44S (GANIL), (β2 (MSU)
Deformation, Modification of the "standard" shell model ?...

4,6,8He+197Au

process
may significantly change the nucleosynthesis scenario

fm
Normal nucleus
consisting of
fermions
Bose
condensate

0+ level of 12C
0.0 0+
4.44 2+
7.65 0+
9.64 3-
7.37
8Be

+ α

First experimental task:
Get evidence of abnormally large dimensions of 7.65 MeV level
The state is unstable

Not reproduced by shell model

Образование элементов тяжелее
гелия происходит путем резонансного слияния трех альфа-частиц.
Увеличение ядерных сил на несколько процентов опустит уровень под порог.
Случайность?
Антропный принцип?

Схема уровней
ядра 12С

Z = N

112Ba (Tretyakova & Ogloblin)

112Ba  nα Q > 0 for n ~ 7
112Ba  3α + 100Sn (double magic core),
Q ~ 13 – 14 MeV
 12C: heavier clustering

Proposal: 112Ba beam and
total cross-section measurements

See rapport A.Ogloblin

the Scientific Council of JINR, Feb.21, 2013, Dubna

of accelerated fission fragments like 132Sn
More intensive beam is needed
160Gd

+ 186W is a good
testing reaction

construction
commissioning
construction
2019
Preparatory phase
SITE?
2020
2021
2022
PHASE1
post acc
CIME
PHASE2
150 AMeV ETUDE
commissioning
NFS
AGATA au GANIL
SPES
Dubna

DRIBs3
ISOL
30A/MeV

Dubna
DRIBs1,2
ISOL
‹10A/MeV

@ 33 AMeV
6Li,15N

@ 46 AMeV
20Ne,32S @ 52 AMeV
… 78Kr @ 41 AMeV

Dubna
Radioactive
Ion
Beams
DRIBs-I → DRIBs-III ↔
2004 2011-2016 > 2018?

RIBs: now
6He@10 AMeV
~5x108 pps

ISOL

Acculinna
1996

Acculinna-2
2015

Production target and ECR source

Combas

RIBs Facilities
@Flerov Lab of Nuclear Reactions, JINR

U400 cyclotron

6- 10 September, 2016
The Topics to be discussed are following:

Rare processes and decays
Methods of production of light exotic
nuclei and study of their properties
Radioactive beams. Production and
research programmes
Experimental set-ups and future
projects
Superheavy elements. Synthesis
and properties

Organized jointly by JINR, GSI, RIKEN, GANIL, NSCL

It is the eight one of a series and is dedicated to the
properties of nuclei in extreme states.

fusion-evaporation with intense n-rich RIB
high-spin spectroscopy
-ray spectroscopy

at S3
in-flight production of exotic nuclei
shape coexistence (at low spin)
low-energy Coulomb excitation
EXOGAM, EUROBALL, AGATA + VASILISA

extrêmes shapes
The nucleus : a laboratory for
fundamental interactions and symmetries
Shell

structure and Isospin
Spin and shapes

TERRA INCOGNITA
( 5000 .. ou .. 7000 !!! )

Key nuclei for
stellar processes are far
from stability

SHE

A new landscape Far of Stability

nuclei
34Ne
35Na
37Mg
39Al
40Al
44Si
45P
31F
22
37Na
38Mg
40Mg
41Al
42Si
43Si
42Al
43Al
45Al
46Si
32
26
34Na
32Ne
33Na
47S
51Ar
49Cl
48S
28
30
34
46P
50Cl
52Ar
51Cl
50S
47P
FRLDM
Mo¨ller, P.,
At. Data Nucl. Data Tables 59,

185–381 (1995).

HFB Goriely, S., et al
Nucl. Phys. A 750, 425–443 (2005).

“Recent observation provides
experimental indication that the neutron drip line may be located further towards heavier isotopes in this mass region than is currently believed.”
T.Baumann et al. Nature 449/25, 2007

Ntot1011c-1

тяжелее
гелия происходит путем резонансного слияния трех альфа-частиц.

Увеличение ядерных сил на

несколько процентов опустит
уровень под порог.

Случайность?
Антропный принцип?

Схема уровней
ядра 12С

“Core” + nα
No

nuclei A  nα, Q > 0 in ground states
Actinide nuclei (A ≥ 220) have Q > 0
for A  nα, n ~ 10.

Dilute surface region of
α’s (“α-halo”), if exists, could contain some properties of
α-condensation matter

Large neutron excess can destroy α-clustering

электромагнитной диссоциации таких ядер предложен новый тип коллективного возбуждения при

малых энергиях возбуждения. Эта новая мода возбуждения была названа “мягким дипольным резонансом”.

Необходимо получить данные о новых более тяжелых ядрах с гало .Пока известны только несколько ядер с двухнейтронным гало (6Не, 8Не,11Li, 14Be и 17В) и всего два ядра с однонейтронным гало (11Be и 19С) . Предсказывается существование многих других галообразных ядер.

Важным с точки зрения структуры и стабильности экзотических ядер является вопрос о последовательности заполнения оболочек. Требует также ответа на вопрос, при каких N и Z происходит заполнение оболочек, какое влияние оказывает спаривание и роль оболочек, в том числе деформированных, на стабильность ядер.

Зависимости радиусов ядер от нейтронного избытка. Использование вторичных пучков радиоактивных ядер позволит определить изоспиновую зависимость пространственного распределения ядерного вещества для многих экзотических ядер

Остается вопрос о корреляциях нуклонов нейтронного гало.Ожидается, что эксперименты с использованием “полной кинематики” могут дать ответ на этот вопрос.

Существование динейтрона и тетранейтрона в ядрах с нейтронным гало а также гало из более крупных кластеров

near the thresholds

A  nα (12C, 16O, …)

Heavy nuclei: systems of the type
“Core” + nα

Энергия возбуждения (МeV/ A)
Experimental dependence of

the nuclear temperature on its excitation energy.

The data were obtained at JINR (Dubna), GSI (Germany) and CERN (Switzerland). Inflections in the curves drawn through the experimental points correspond to a phase transition «liquid-gas».

F-Ne-Na Neutron Nuclei

beams
RIB facilities
ISOLDE, FAIR, SPIRAL 2, EURISOL, DRIBs
RIB

physics
Nuclear structure
Nuclear reactions
Nuclear Astrophysics
Why do we need high intensity RIB?