Evgeniya Kravchenko

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Evgeniya Kravchenko XI Russian-Finnish Symposium
on Radio Astronomy October 19, 2010 Pushchino,
Russia
Ultra High Energy Neutrinos and radio method of
its registration
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I have done a terrible thing. I have postulated
a particle that cannot be detected
Wolfgang Pauli
Evgeniya Kravchenko, XI RFSRA, 2010
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Electromagnetic Weak Strong Gravitation
Radio, optic, IFR, X-rays, UV
leptons, hadrons gluons, quarks bozons Higgs-bozon
Topological deffects, strings
interactions
Evgeniya Kravchenko, XI RFSRA, 2010
Gravitons
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Cosmic Rays
Cosmic rays with 21020 eV according ?s 700 TeV
LHC work up to 14 TeV according 81016 eV
Evgeniya Kravchenko, XI RFSRA, 2010
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Cosmic Rays
The current data set has 17333 events between 0.1
and 41.1 EeV. Last event has been recorded on Jun
08 2010 052438, UTC Time (PAO).
Evgeniya Kravchenko, XI RFSRA, 2010
Evidence for proton-dominated cosmic ray
composition above 1.6 EeV ,The HiRes
collaboration, arXiv0910.4184
The Pierre Auger Observatory a new stage in
the study of the ultra high energy cosmic rays
,Serguei Vorobiev, arXiv0811.0752
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Correlations?
Evgeniya Kravchenko, XI RFSRA, 2010
- galaxies with radio jets at D75 Mpc -
galaxies with radio jets at 75 Mpc lt D 200 Mpc
- galaxies with radio jets at 200 Mpc lt D 500
Mpc ? - Galactic SGRs ? - AXPs
O - 56-75 1018 eV UHECRs by PAO O - gt75 1018 eV
UHECRs by PAO O - AGASA UHECRs events of radius
3.50
Ultra-High Energy Cosmic Rays Detected by Auger
and AGASA Corrections for Galactic Magnetic
Field Deflections, Source Populations, and
Arguments for Multiple-Components, Neil M. Nagar
and Javier Matulich anhiarXiv0912.2131
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Peculiarities
TeV Strings and the Neutrino-Nucleon Cross
Section at Ultra-high Energies, F. Cornet,
arXivhep-ph/0102065
mvlt1eV neutral stable weakly interacting
Evgeniya Kravchenko, XI RFSRA, 2010
not deflected ? point back to the source not
absorbed ? travel Gpc distances
At 5 Gpc probability to interact is lt5
s10-66 ?m-2s10-52 ?m-2 s10-47 ?m-2s810-34
?m-2
relic neutrino background
Z0W
s10-34 ?m-2s4.210-32 ?m-2
At ?v1021 eV and mv1eV s10-42 ?m-2
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Sources
Scenarios
Top-down
Bottom-up
decay or annihilation
acceleration
Evgeniya Kravchenko, XI RFSRA, 2010
1-10 MeV
Decay of massive X particles Topological
defects Cosmic strings Superconductive
strings Magnetic monopoles Cosmic
loops Vortons Z-bursts
gt TeV
Active Galaxies Nucleus Gamma Ray
Bursts GZK-neutrinos Magnetars, Neutron stars
Binaries Spiral galaxies Supernovae
explozion Supernovae remnant Microquasars
Topological defects predict that
the highest-energy cosmic rays are predominantly
protons
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GZK-neutrinos
Greizen-Zatsepin-Kuzmin (GZK) cut-off at 61019
eV Lint lt 50Mpc
Evgeniya Kravchenko, XI RFSRA, 2010
412 ?cmb per cm-3
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Fluxes
Evgeniya Kravchenko, XI RFSRA, 2010
GZK-v flux ?1019 lt 1 particles\?m2\year ?1020
lt 1 particle\1 ?m2\100 year
Huge Volumes!
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• Methods

Different neutrino registration methods
Optical Cherenkov emission
Radio Cherenkov emission
Acoustic Cherenkov emission
Extensive Air Showers
Space
Water
Ice
Earth-based
Earth-based
Space
EUSO OWL
IceCube
Baikal ANTARES NEMO NESTOR (KM3Net)
ANTARES IceCube
PAO
RESUN GLINT Astropeiler NuMoon GMRT RICE SalSa ARI
ANNA ARA LunaSKA LOFAR
ANITA LORD
Evgeniya Kravchenko, XI RFSRA, 2010
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Askaryan Effect
Was predicted at 1965 by Gurgen Askaryan Was
confirmed in 2000 on SLAC
? e-at ? ? e- e e-at ? e e- e- e-at ?
e- e- e e-at ? ? ?
Evgeniya Kravchenko, XI RFSRA, 2010
Attenuation length at 1GHz in Moon regolith is 18
m Ice is 1 km
Shower length 1.5 m Lateral size of cascade
10 cm Coherent up to 3GHz The duration of the
shower 2-6 ns
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Coherent Radio Emission from Cosmic Showers in
Air and in Dense Media, Askar'yan, G. A.,
Soviet Physics JETP, Vol. 21, p.658, 1965
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Evgeniya Kravchenko, XI RFSRA, 2010
MOON
Radio Cherenkov Emission
GLUE 2004
Parkes 2007
Kalyazin 2005
GMRT
NuMoon
GLINT
RESUN
LOFAR LunaSKA (ATCA) SKA
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Radio Cherenkov emission
SalSa
ARA
RICE
AURA
ANITA
Evgeniya Kravchenko, XI RFSRA, 2010
Auger (1y) 3103 ?m2 1
IceCube (3y) 1 ?m3 0.3
ANITA (45d) 106 ?m3 lt1
SalSa ( 3y) 3103 ?m3 lt50
Cosmic rays are protons
ARIANNA
Radio Detection of GZK Neutrinos - AURA status
and plans, H. Landsman etc, Proceedings of the
30th International Cosmic Ray Conference, Vol. 4,
p827830
Simulation of the Event Reconstruction of Ultra
High Energy Cosmic Neutrinos with Askaryan Radio
Array, Shang-Yu Sun, Pisin Chen and Melin Huang,
2010, arXiv1002.0023
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RITA
SKA gt2000 LOFAR (Dutch)
52 ANITA (3 flights) 32 ARIANNA
gt200 KM3Net 300 IceCube
271 Auger 85 SalSa
125 KM3Net lt200 ARA 8
Radio Ice Tethered Antenna in Antarctica

• D. Besson
• R. Dagkesamanskii
• E. Kravchenko
• Kravchenko
• I. Zheleznykh

University of Kansas Pushchino RAO ASC
LPI University of Nebraska Institute of Nuclear
Research RAS
4-5 arrays 16 dipoles in each 760 MHz bandwidth
120MHz Sensivity 1 MJy or 0.13 ?V/m/MHz Height
1-3 km over ice near the Vostok Station Ice
depth to 3.5 km Effective Target Volume 50 km3
(1019 eV) Planned time exposure 180 days Number
of balloons 5 Maximum neutrino flux at 51019
eV
Evgeniya Kravchenko, XI RFSRA, 2010
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RITA
760 MHz Sensivity 0.9 Mjy Height 3 km over
the ice Time exposure 180/360 days Number of
balloons 1
Evgeniya Kravchenko, XI RFSRA, 2010
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Fermi-LAT restrictions on UHECRs and cosmogenic
neutrinos, V. Berezinsky, A. Gazizov et al.,
arXiv1003.1496
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LORD
Lunar Orbital Radio Detector
Evgeniya Kravchenko, XI RFSRA, 2010
Detection of Ultrahigh-Energy Cosmic Rays and
Neutrinos by Radio Method Using Artificial Lunar
Satellites, G. A. Gusev, Cosmic Research, 2006,
Vol. 44, No. 1, pp. 1938
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For what?
Neutrino Cross section Elementary particle
physics on PeV-EeV scale Heavy dark matter
content in the Universe Active galaxies
phase Particle acceleration mechanism in
astrophysical sources - AGN GRB SN BH
Evgeniya Kravchenko, XI RFSRA, 2010
SN1987A
Markarian 501 136 Mpc
1013 eV ? Lint 70 Mpc
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Thank Y for patience
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Extra slides
Paolo Lipari, VLVnT, Athens 12th October 2009