JINR astrophysical studies JINR astrophysical studies in the in the NUCLEONNUCLEON andand TUS TUS

space experimentsspace experiments

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Galactic:supernova remnants?

extragalactic:gamma ray

bursts?ТUS

NUCLEON

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NUCLEON experiment statusNUCLEON experiment status

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SINP MSU, Moscow “Gorizont”, Ekaterinburg НИИ Материаловедения, Zelenograd JINR, Dubna Frunze Arsenal Design Bureau, St.-Petersburg

Knee

Прямыеизмерения

There is a large difference in data for the CR nuclear component flux and composition around of the knee region

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Эксперимент АМЭксперимент АМS-2S-2

Galactic cosmic ray anisotropyGalactic cosmic ray anisotropy

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The arrival direction of cosmic-ray muons recorded with 40 IceCube strings (Southern Hemisphere). The variations are of order 10−3 on a uniform distribution. The color scale represents the relative intensity. The dots indicate the directions of Vela and Geminga - the brightest gamma-ray sources in the sky. Also shown is the muon data of Milagro obtained by the same method (Northern Hemisphere). Muon energy ≈ 20 ТэВ. The anisotropy contradicts to the average value of the galactic magnetic fields about of fewμG: charge particle giroradius is ~0.1 pc for E ~ 100 TeV, distance up to Vela ~ 100 pcthat is possible source of GCR. NUCLEON provides good statistics to study anisotropy.

Medium scale anisotropy

IceCube

Milagro

NUCLEON

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NUCLEON apparatus consists of- NUCLEON detector as a monoblock inside of pressure container,- Special telemetry system inside of separate container, - Antenna-fider system,- Mechanical support interface of the connection with base satellite

system.

Main NUCLEON parameters:-Total weight ~ 350 kg (for detector ~250 kg);- Power cunsumtion~150 W (for detectors ~ 120 W);- Telemetry ~270 MB/day;- Data taking period ≥5 years.

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NUCLEONNUCLEON detector detector

+ microcalorimeter

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The NUCLEON apparatus in assemble before combine tests

Beam testBeam testss at at SPS SPS CERN – 2011CERN – 2011-2013-2013

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NUCLEON charge measuring test at 2013 CERN

New NUCLEON cip test at 2013 CERN

Proton spectrum to be expected in the NUCLEON experiment (green crosshatched region)

NUCLEON 3 year data taking

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Conclusion - NUCLEONConclusion - NUCLEON

The The flight NUCLEON flight NUCLEON copy copy was producedwas produced, tested at SPS , tested at SPS CERNCERN in 2011 in 2011-2013 -2013 and is ready for assembling at the and is ready for assembling at the RESURS P №2 satelliteRESURS P №2 satellite. .

The The NUCLEON missionNUCLEON mission is is planned for operation planned for operation since since the the 20142014 for for 3 -5 years of data taking3 -5 years of data taking

Next step is Next step is HEROHERO experimentexperiment. .

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Ultra High Energy Cosmic RaysUltra High Energy Cosmic Rays TUS experiment statusTUS experiment status

Е Е >> 4*10 4*1019 19 эВэВ

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- Skobeltsyn Institute of Nuclear Physics, MSU, Moscow, Russia - Joint Institute for Nuclear Research - Space Regatta Consortium, Korolev, Moscow region, Russia - Physics Department, EWHA Woman University, Seoul, Korea - University of Puebla, Puebla, Puebla, Mexico - University of Michiocan, Morelia, Michiocan, Mexico

The fluorescence EAS radiation may be measured by the ground or space detectors to get the longitudinal shower profile and obtain the UHECR parameters: energy, arrival direction and nature (proton or nuclear). A Cerenkov radiation reflected fromthe Earth surface or clouds may be measured from space also. Atmospheric conditions are much more stable in upper layers of the atmosphere thatis important to reduce systematic uncertainty of the UHECR energy measurement.

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CRISIS 2009: MASS COMPOSITION

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HiRES

Auger

The main problems in UHECR:

• mass composition at 1 × 1018 − 1 × 1020 eV.• origin of cutoff at E ~ 5 × 1019 eV (GZK cutoff ?)• DETECTION OF UHE GZK NEUTRINOS.• search for the UHECR sources.• theory of acceleration to the highest energies.

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The TUS is the main detector at the “Mikhail Lomonosov” satellite

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TUS will measure the EASfluorescent radiation

JINR responsibilityJINR responsibility: Fresnel : Fresnel mirror production, tests and mirror production, tests and

optical parameter measurementsoptical parameter measurements

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The TUS Fresnel mirror.

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Left: The Point Spred Function (PSF) angular dependence of the ideal TUS Fresnel mirrorRight: The PSF angular dependence of the real TUS Fresnel mirror.

The optical parameters measurement

TUS test at the ISTRA space center

TUS calibration in flight The UV light source on the drone or plane is the only possibility

Conclusion - TUSConclusion - TUS

The The TUS mirrorTUS mirrorss w wereere produced andproduced and tested in 2010 tested in 2010-2012-2012. It . It confirms reliability of the mirror confirms reliability of the mirror design: design: carbon plastic and carbon plastic and aluminum honeycomb.aluminum honeycomb.

The The optical parametersoptical parameters of the mirror are of the mirror are measured and are measured and are in in reasonable correspondence as with the reasonable correspondence as with the Field-of-View Field-of-View of the of the TUS photo receiver as with PMT TUS photo receiver as with PMT pixel sizepixel size

The The flight flight TUSTUS model model is ready for integration at the is ready for integration at the Mikhail Mikhail Lomonosov Lomonosov satellite. . satellite. .

The The TUS missionTUS mission is is planned for operation planned for operation inin 20120144 for for 3 years 3 years of data takingof data taking

TUS is the pilot experimentTUS is the pilot experiment to confirm a possibility UHECR to confirm a possibility UHECR study from spacestudy from space. . Next step is Next step is KLYPVEKLYPVE experiment on ISSexperiment on ISS. .

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