Evgeniya Kravchenko XI RussianFinnish Symposium on Radio Astronomy

Evgeniya Kravchenko XI Russian-Finnish Symposium on Radio Astronomy October 19, 2010 Pushchino, Russia Ultra High Energy Neutrinos and radio method of its registration

Evgeniya Kravchenko, XI RFSRA, 2010 “I have done a terrible thing. I have postulated a particle that cannot be detected” Wolfgang Pauli 1

Evgeniya Kravchenko, XI RFSRA, 2010 Radio, optic, IFR, X-rays, UV leptons, hadrons gluons, quarks bozons Higgs-bozon Topological deffects, strings Gravitons Electromagnetic Weak interactions Strong Gravitation 2

Evgeniya Kravchenko, XI RFSRA, 2010 Cosmic Rays Cosmic rays with 2*1020 e. V according s = 700 Te. V LHC work up to 14 Te. V according 8*1016 e. V 3

Evgeniya Kravchenko, XI RFSRA, 2010 Cosmic Rays The current data set has 17333 events between 0. 1 and 41. 1 Ee. V. Last event has been recorded on Jun 08 2010 05: 24: 38, UTC Time (PAO). “Evidence for proton-dominated cosmic ray composition above 1. 6 Ee. V” , The Hi. Res collaboration, ar. Xiv: 0910. 4184 “The Pierre Auger Observatory – a new stage in the study of the ultra high energy cosmic rays” , Serguei Vorobiev, ar. Xiv: 0811. 0752 4

Evgeniya Kravchenko, XI RFSRA, 2010 Correlations? O - 56 -75 1018 e. V UHECRs by PAO O - >75 1018 e. V UHECRs by PAO O - AGASA UHECRs events of radius 3. 5 0 • - galaxies with radio jets at D~75 Mpc • - galaxies with radio jets at 75 Mpc < D 200 Mpc • - galaxies with radio jets at 200 Mpc < D 500 Mpc - Galactic SGRs - AXPs “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 anhiar. Xiv: 0912. 2131 5

Evgeniya Kravchenko, XI RFSRA, 2010 Peculiarities “Te. V Strings and the Neutrino-Nucleon Cross Section at Ultra-high Energies”, F. Cornet, ar. Xiv: hep-ph/0102065 mv<1 e. V neutral stable weakly interacting not deflected point back to the source not absorbed travel Gpc distances At 5 Gpc probability to interact is <5% relic neutrino background: s=10 -66 сm-2 s=10 -52 сm-2 s=10 -47 сm-2 s=8· 10 -34 сm-2 Z 0 s=10 -34 сm-2 -32 -2 W± s=4. 2· 10 сm At Еv~1021 e. V and mv=1 e. V s~10 -42 сm-2 6

Sources Top-down: Scenarios Bottom-up: decay or annihilation Evgeniya Kravchenko, XI RFSRA, 2010 acceleration Decay of massive “X” particles Topological defects: Cosmic strings Superconductive strings Magnetic monopoles Cosmic loops Vortons Z-bursts Topological defects predict that the highest-energy cosmic rays are predominantly protons > Te. V Active Galaxies Nucleus Gamma Ray Bursts GZK-neutrinos Magnetars, Neutron stars 1 -10 Me. V Binaries Spiral galaxies Supernovae explozion Supernovae remnant Microquasars 7

Evgeniya Kravchenko, XI RFSRA, 2010 GZK-neutrinos 412 cmb per cm-3 Greizen-Zatsepin-Kuzmin (GZK) cut-off at 6*1019 e. V Lint < 50 Mpc 8

Evgeniya Kravchenko, XI RFSRA, 2010 Fluxes GZK-v flux Е=1019 < 1 particlesкm 2year Е≥ 1020 < 1 particle1 кm 2100 year Huge Volumes! 9

Evgeniya Kravchenko, XI RFSRA, 2010 Methods Different neutrino registration methods Optical Cherenkov emission Water Baikal ANTARES NEMO NESTOR (KM 3 Net) Acoustic Extensive Air Showers Cherenkov emission Space Ice. Cube ANTARES Ice. Cube EUSO OWL Earth-based PAO Radio Cherenkov emission Space ANITA LORD Earth-based RESUN GLINT Astropeiler Nu. Moon GMRT RICE Sal. Sa ARIANNA ARA Luna. SKA LOFAR 10

Evgeniya Kravchenko, XI RFSRA, 2010 Askaryan Effect Was predicted at 1965 by Gurgen Askaryan Was confirmed in 2000 on SLAC + e-at + ee+ + e-at e+ + ee- + e-at e- + ee+ + e-at + Attenuation length at 1 GHz in Moon regolith is 18 m Ice is 1 km Shower length ~ 1. 5 m Lateral size of cascade ~ 10 cm Coherent up to ~3 GHz The duration of the shower ~ 2 -6 ns 11 “Coherent Radio Emission from Cosmic Showers in Air and in Dense Media”, Askar'yan, G. A. , Soviet Physics JETP, Vol. 21, p. 658, 1965

Evgeniya Kravchenko, XI RFSRA, 2010 MOON GLUE Radio Cherenkov Emission Parkes 2007 Kalyazin 2005 2004 GMRT Nu. Moon GLINT RESUN LOFAR Luna. SKA (ATCA) SKA 12

Radio Cherenkov emission Sal. Sa ARA RICE AURA Evgeniya Kravchenko, XI RFSRA, 2010 ANITA Auger (1 y) 3*103 кm 2 1 Ice. Cube (3 y) 1 кm 3 0. 3 ANITA (45 d) 106 кm 3 <1 Sal. Sa ( 3 y) 3*103 кm 3 <50 Cosmic rays are protons ARIANNA “Radio Detection of GZK Neutrinos - AURA status and plans”, H. Landsman etc, Proceedings of the 30 th International Cosmic Ray Conference, Vol. 4, p 827– 830 “Simulation of the Event Reconstruction of Ultra High Energy Cosmic Neutrinos with Askaryan Radio Array”, Shang-Yu Sun, Pisin Chen and Melin Huang, 2010, ar. Xiv: 1002. 0023 13

RITA Radio Ice Tethered Antenna in Antarctica Evgeniya Kravchenko, XI RFSRA, 2010 D. Besson R. Dagkesamanskii E. Kravchenko II. I. Zheleznykh University of Kansas SKA LOFAR (Dutch) ANITA (3 flights) ARIANNA KM 3 Net Ice. Cube Auger Sal. Sa KM 3 Net ARA >$2000 € 52 $32 >$200 € 300 $271 € 85 $125 <€ 200 $8 Pushchino RAO ASC LPI 1. 2. University of Nebraska Institute of Nuclear Research RAS 4 -5 arrays 16 dipoles in each 760 MHz bandwidth 120 MHz 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 km 3 (1019 e. V) Planned time exposure: 180 days Number of balloons: ~ 5 Maximum neutrino flux at ~5*1019 e. V 14

Evgeniya Kravchenko, XI RFSRA, 2010 RITA 760 MHz Sensivity: 0. 9 Mjy Height: 3 km over the ice Time exposure: 180/360 days Number of balloons: 1 “Fermi-LAT restrictions on UHECRs and cosmogenic neutrinos”, V. Berezinsky, A. Gazizov et al. , ar. Xiv: 1003. 1496 15

Evgeniya Kravchenko, XI RFSRA, 2010 LORD Lunar Orbital Radio Detector “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. 19– 38 16

Evgeniya Kravchenko, XI RFSRA, 2010 For what? Neutrino Cross section Elementary particle physics on Pe. V-Ee. V scale Heavy dark matter content in the Universe Active galaxies’ phase Particle acceleration mechanism in astrophysical sources - AGN & GRB & SN & BH SN 1987 A 1013 e. V Lint ~ 70 Mpc Markarian 501 136 Mpc 17

Thank Y for patience

Extra slides Paolo Lipari, VLVn. T, Athens 12 th October 2009