1 / 20

Evgeniya Kravchenko XI Russian-Finnish 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. “ I have done a terrible thing. I have postulated a particle that cannot be detected ” Wolfgang Pauli.

vanig
Télécharger la présentation

Evgeniya Kravchenko XI Russian-Finnish Symposium on Radio Astronomy

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

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

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

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

  4. Cosmic Rays Cosmic rays with 2*1020eV according s = 700 TeV LHC work up to 14 TeV according 8*1016eV EvgeniyaKravchenko, XI RFSRA, 2010 3

  5. 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 05:24:38, UTC Time (PAO). EvgeniyaKravchenko, XI RFSRA, 2010 “Evidence for proton-dominated cosmic ray composition above 1.6 EeV” ,The HiRes collaboration, arXiv:0910.4184 “The Pierre Auger Observatory – a new stage in the study of the ultra high energy cosmic rays” ,Serguei Vorobiev, arXiv:0811.0752 4

  6. Correlations? EvgeniyaKravchenko, XI RFSRA, 2010 • - 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 O - 56-75 1018 eV UHECRs by PAO O - >75 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 anhiarXiv:0912.2131 5

  7. Peculiarities “TeV Strings and the Neutrino-Nucleon Cross Section at Ultra-high Energies”, F. Cornet, arXiv:hep-ph/0102065 mv<1eV neutral stable weakly interacting EvgeniyaKravchenko, XI RFSRA, 2010 not deflected  point back to the source not absorbed  travel Gpc distances At 5 Gpc probability to interact is <5% s=10-66сm-2s=10-52 сm-2s=10-47сm-2s=8·10-34сm-2 relic neutrino background: Z0W± s=10-34 сm-2s=4.2·10-32 сm-2 At Еv~1021eV andmv=1eVs~10-42 сm-2 6

  8. Sources Scenarios Top-down: Bottom-up: decay or annihilation acceleration EvgeniyaKravchenko, XI RFSRA, 2010 Decay of massive “X” particles Topological defects: Cosmic strings Superconductive strings Magnetic monopoles Cosmic loops Vortons Z-bursts >TeV 1-10 MeV 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 7

  9. GZK-neutrinos Greizen-Zatsepin-Kuzmin (GZK) cut-off at 6*1019eV Lint < 50Mpc EvgeniyaKravchenko, XI RFSRA, 2010 412 cmb per cm-3 8

  10. Fluxes EvgeniyaKravchenko, XI RFSRA, 2010 GZK-v flux Е=1019< 1particles\кm2\year Е≥1020< 1 particle\1кm2\100 year Huge Volumes! 9

  11. Different neutrino registration methods Optical Cherenkov emission Acoustic Cherenkov emission Radio Cherenkov emission Extensive Air Showers Methods Space Water Ice Earth-based Space Earth-based EUSO OWL Baikal ANTARES NEMO NESTOR (KM3Net) IceCube ANTARES IceCube PAO RESUN GLINT Astropeiler NuMoon GMRT RICE SalSa ARIANNA ARA LunaSKA LOFAR EvgeniyaKravchenko, XI RFSRA, 2010 ANITA LORD 10

  12. 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 +  EvgeniyaKravchenko, 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 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

  13. EvgeniyaKravchenko, XI RFSRA, 2010 MOON Radio Cherenkov Emission GLUE 2004 Parkes 2007 Kalyazin 2005 GMRT NuMoon GLINT RESUN LOFAR LunaSKA (ATCA) SKA 12

  14. Radio Cherenkov emission SalSa ARA RICE AURA ANITA EvgeniyaKravchenko, XI RFSRA, 2010 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, p827–830 “Simulation of the Event Reconstruction of Ultra High Energy Cosmic Neutrinos with Askaryan Radio Array”, Shang-Yu Sun, Pisin Chen and Melin Huang, 2010, arXiv:1002.0023 13

  15. RITA SKA >$2000 LOFAR (Dutch) €52 ANITA (3 flights) $32 ARIANNA >$200 KM3Net €300 IceCube $271 Auger €85 SalSa $125 KM3Net <€200 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 MJyor 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 ~5*1019 eV EvgeniyaKravchenko, XI RFSRA, 2010 14

  16. RITA 760 MHz Sensivity: 0.9Mjy Height: 3 km over the ice Time exposure: 180/360 days Number of balloons: 1 EvgeniyaKravchenko, XI RFSRA, 2010 “Fermi-LAT restrictions on UHECRs and cosmogenic neutrinos”, V. Berezinsky, A. Gazizov et al., arXiv:1003.1496 15

  17. LORD Lunar Orbital Radio Detector EvgeniyaKravchenko, 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. 19–38 16

  18. 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 EvgeniyaKravchenko, XI RFSRA, 2010 SN1987A Markarian 501 136 Mpc 1013 eV Lint ~ 70 Mpc 17

  19. Thank Y for patience

  20. Extra slides Paolo Lipari, VLVnT, Athens 12th October 2009

More Related