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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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