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Joint Institute for Nuclear Research
Dzhelepov Laboratory of Nuclear Problems
Georgy SHELKOV
Students Practice in JINR Field of Research
Dubna, 08 July 2013
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We are
here
JINR comprises 7 Laboratories, each being
comparable with a large institute in the scale and scope
of investigations performed
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Veksler and Baldin
Laboratory of High Energy Physics Dzhelepov
Laboratory of Nuclear Problems
Bogoliubov
Laboratory of Theoretical Physics
Frank Laboratory of Neutron Physics
Flerov
Laboratory of Nuclear Reactions
Laboratory of
Information Technologies
Laboratory of Radiation Biology
Dzhelepov Laboratory of Nuclear Problems
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First accelerator in Dubna
World largest 680 MeV proton synchrocyclotron
was launched December 14, 1949
M.Mescherjakov V.Dzhelepov
Basic Scientific Directions
DLNP
Neutrino Physics
High Energy Physics
Nuclear Physics
Physics instruments and methods
Develop and transfer of New Technologies
Training of young staff
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Basic Scientific Directions
DLNP
Neutrino Physics
High Energy Physics
Nuclear Physics
Physics instruments and methods
Develop and transfer of New Technologies
Training of young staff
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Neutrino Physics at JINR has started with
Bruno Pontecorvo
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Study of Neutrino mixing parameters (OPERA, Daya Bay)
Search for Neutrinoless Double beta decay (SuperNEMO, Gerda)
Development of neutrino detection technique and experiments at KNPP
(GEMMA, DANSS)
Solar and Astro neutrino experiments (BAIKAL, Borexino)
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Key measurements with DLNP JINR participation:
Why neutrino is the main
“newsmaker” at particle physics
now?
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The Four Fundamental Forces
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How we detect elementary particles?
•All objects of particle physics study (elementary
particles) are invisible for us and we can see only the
results of their interaction with matter by one of
mentioned above fundamental interaction.
•“Most comfortable” for registration are particles which
can interact by electromagnetic (ionization losses and
so on) or strong interaction.
•“Most difficult” to detect particles by weak interaction.
•Neutrino is an object which interacted by weak
interaction only and therefore very difficult to detect it 12
What we know about neutrinos?
Quarks u c t ?
d s b ?
Leptons e μ τ ?
νe νμ ντ ?
Generation I II III IV
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LEP results
•15.05.12 •14
JINR was active member of DELPHI
What we know about neutrinos?
Quarks u c t ?
d s b ?
Leptons e μ τ ?
νe νμ ντ ?
Generation I II III IV
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What we know about neutrinos?
Charge Spin Mass
νe 0 1/2 < 2 eV
νμ 0 1/2 < 0,19 MeV
ντ 0 1/2 < 18,2 MeV
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Neutrino Astronomy
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Ice as a natural deployment platform
• Ice stable for 6-8 weeks/year:
– Maintenance & upgrades
– Test & installation of new equipment
Winches used for deployment
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The NT-200 Telescope
• I.Belolaptikov
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-8 strings: 72m height
- 192 optical modules
pairwise coincidence
96 space points
calibration with N-lasers
timing ~ 1 nsec
- Dyn. Range ~ 1000 pe Effective area: 1 TeV ~2000 m²
Eff. shower volume: 10TeV ~0.2Mt
Quasar PMT: d = 37cm Height x = 70m x 40m,
Vgeo=105m3= 0.1Mton
•15.05.12 •28
Baikal detector -II
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The next step is construction of 1 км3
BAIKAL Detector ,
2014 – 2016 – first stage (0.1 – 0.3) км3
2017 – second stage (0.3 – 0.6) км3
2018 – third stage (0.6 – 0.9) км3
Which will consist of 2400 optical elements, combined in clusters with 8 strings of optical elements each
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Neutrino Astronomy
•15.05.12
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It is well understood that detection of neutrino brings an important information complementary to the traditional optic and radio telescopes.
An important tool is the BAIKAL neutrino telescope, which can measure : point-like sources , diffused neutrino fluxes , neutrino from annihilation of dark matter, new exotic particles like monopoles, and many others.
Present results are
obtained with NT200+
(192 elements on 8
strings)
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The history of cooperation between CERN and JINR spans over 49 years.
1963, JINR, Dubna
CERN DG Prof. V.Weisskopf,
Profs. V.Dzhelepov and
B.Pontecorvo
1971, Dubna
CERN DG
and JINR Director
Prof. W.Jentschke
Prof. N.Bogoliubov
JINR physicists are widely involved in leading CERN projects, including 3 experiments at the LHC
High Energy Physics
Experiments at LHC: ATLAS
DLNP JINR participates in:
Higgs Physics
QCD and SM Physics
Top quark Physics
SUSY Physics
Exotics Physics
Heavy Ions Physics
ATLAS
Conclusion #1
Astroparticle physics in general, and neutrino physics in particular, represent today the most intriguing field, where possible new physics is expected
There is an important contribution from JINR and its Member States to this field in the experimental, theoretical and technological areas
The existing and planned experiments with JINR participation provide the basis for continuation of this interesting and promising program
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Basic Scientific Directions
DLNP
Neutrino Physics
High Energy Physics
Nuclear Physics
Physics instruments and methods
Develop and transfer of New Technologies
Training of young staff
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Semiconductor detectors R&D at DLNP
and possible spin off
Principle of semiconductor detector operation
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The most widespread material for a sensor - silicon (Si) in force:
• low cost of initial raw materials (SiO2 sand)
• existence of technology of mass production
Incoming particles:
Charge
Gamma
Electrical signal
Sensor
Amplifier
Discriminator
Digitization
Electronics
Analyze
•ATLAS pixel
80 million channels in a clilnder 1,4
m long and 0,5 m in diameter
... dissipating more than 15 kW
Disadvantages of Si sensors
Relatively low radiation hardness
JINR group is doing R&D with GaAs since 2006
Obviously we have started from HEP motivation - R&D
for using GaAs as a radiation hard material for the
forward calorimeter in the frame of ILC R&D together
with DESY (Zeuthen) colleagues
A lot of sensors from different variants of
GaAs:Cr were ordered for R&D by JINR
and produced at TSU (Tomsk)
Possible spin-off
Quite soon we have recognized that
GaAs:Cr is very promising material as a
gamma ray sensor with possible
application in biomedicine and geology
Disadvantages of Si sensors
Relatively low radiation hardness
Low efficiency of gamma ray
registration (Z=12)
Till now very limited number of new high-Z
materials for sensors is available. Most advanced are:
GaAs(Z~32), CdTe(Z~49)
We will talk now about GaAs
It must be emphasized that this material is made exclusively in Russia
Incoming particles:
Charge
Gamma
Electrical signal
Sensor
Amplifier
Discriminator
Digitization
Electronics
What is X-ray diagnostic method today?
Classical scheme of X-ray diagnostic
From 2D roentgenogram to 3D CT
One CT slice is the result of joint processing of
a large number of roentgenogram obtained at
rotation around an object
Voxel X-ray tube
Slice image
Rotation
Detector
Sensors for X-ray imaging systems The best X-ray imaging systems on the market today
are pixel detector with indirect conversion -
(scintillator + Si photo detector)
Much better properties (conversion efficiency, spatial
resolution) has a direct conversion detector with solid
pixel sensor
Modern Pixel detector for X-ray imaging
Sensor
Read out chips
Last batch of detectors
From B&W roentgenogram to color one! “Color” means energy sensitive
From B&W roentgenogram to color one!
“Color” means energy sensitive
New generation of X-ray pixel detectors
(GaAs:Cr + energy sensitive in photon
counting mode @ RO electronic chips)
gives new prospects for X-ray tomography
diagnostic development.
K-edge method
Let’s assume that our object consist from (Water + Calcium +Gadolinium)
Kabsorption(object)=Kabs (H2O)+Kabs (Ca)+Kabs(Gd)
At energy =Scan1: Kabs(object)1=Kabs (H2O)1+Kabs (Ca)1+Kabso(Gd)1
At energy =Scan2: Kabs(object)2=Kabs (H2O)2+Kabs (Ca)2+Kabs(Gd)2
Kabs (H2O)1≈Kabs (H2O)2; Kabs (Ca)1≈Kabs(Ca)2 BUT Kabs(Gd)2>>Kabso(Gd)1
It means that:
Image(2)-Image(1) ~ Image of Gd (!)
Micro-tomograph MARS
Micro-tomography images of mouse obtained in
University of Canterbury Christchurch New Zealand
with MARS micro-tomograph
Micro-tomography images of mouse obtained in
University of Canterbury Christchurch New Zealand
with MARS micro-tomograph
The MARS micro-tomograph for DLNP is on
the way from New Zealand to Dubna and
should start to work in 2013.
We invite interested physicist and physician
to joint us at R&D of new detectors and the
X-ray computed tomography methods
Thank you for your
attention
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Back up slides
•JINR is responsible for the electronic detectors analysis and the neutrino
interaction vertex location prediction for all the events
•Aim of OPERA is Appearance
detection
•LNGS
•Present Analysis (~30% of Data):
• 2 candidate events observed
• 2.1 signal and
• 0.2 background events expected
JINR in OPERA experiment
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JINR in Daya Bay experiment
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Weighted Baseline [km]
0 0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 1.8 2
expec
ted
/ N
det
ecte
dN
0.9
0.95
1
1.05
1.1
1.15
EH1 EH2
EH3
13q22sin
0 0.05 0.1 0.15
2c
0
10
20
30
40
50
60
70
s1s3
s5
•sin22θ13 = 0.089 ± 0.010 (stat) ± 0.005
(syst)
• Interpretation of far/near disappearance yields the most precise
to date measurement of:
•6 commercial reactor cores
•with 17.4 GW total power.
•6 Antineutrino Detectors (ADs)
•give 120 tons total target mass.
•Data from
•24/12/2011 to 11/05/2012
•~200K events
•in near detectors
•~30K events
•in far detectors
TEXONO (2006):
< 7.4 10 –11 B
GEMMA I (2006):
< 5.8 10 –11 B
BOREXINO (2008)
< 5.4 10 –11 B
GEMMA I+II (2009):
< 3.2 10 –11 B The Best limit!
•Search for Neutrino Magnetic moment
measurement with JINR detector GEMMA
Neutrinos at Kalinin
Power Plant
•Configuration: 96 Strings × 24 OM
• Instr. Volume 0.3 km3
•Expected parameters:
• Effective cascade volume
• Cascade energy >100TeV
• Veff = 0.1– 0.7km3,
• δ(lgE) ~ 0.1, θmed ~ 5o-7o
• Effective muon area
• Muon energy >3 TeV
• Seff ~ 0.1– 0.8 km2,
• δ(lgE) ~ 0.4, θmed ~ 0.5o
•Str
ing
sec
tio
n,
12
OM
•R ~ 60 m
•L~
350 m
•12 clusters of strings
•1 km
•Central Physics Goals:
Investigate Galactic and extragalactic neutrino “point
•sources” in energy range > 3 TeV
Diffuse neutrino flux – energy spectrum, local and global
•anisotropy, flavor content
Transient sources (GRB, …)
Dark matter – indirect search
Exotic particles – monopoles, Q-balls, nuclearites, …
•Status: TDR is ready (2011) Prototype string tested (2009-2010) Data analysis shows good consistency. New optical cable was mounted (2011) Prototype cluster (3 strings) is operating now •67
Neutrino astrophysics. Baikal project: Gigaton Volume Detector (GVD)
•Baikal deep underwater neutrino telescope НТ – 200+
“Baikal” is INR-JINR common
project
JINR in some figures JINR’s staff members ~ 4500
researchers ~ 1200
including from the Member States (but Russia) ~ 400
Doctors and PhD ~ 1000
JINR Budget
(actual and foreseen
in the 7-year Plan)
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50
100
150
200
250
2010 2011 2012 2013 2014 2015 2016
M$
International collabiraton JINR collaborates with more than 700 scientific centres
and universities in 63 countries of the world.
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