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XIII International Symposium on Very High Energy Cosmic Ray Interactions

XIII International Symposium on Very High Energy Cosmic Ray Interactions Pylos, 6 -12 September 2004.

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XIII International Symposium on Very High Energy Cosmic Ray Interactions

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  1. XIII International Symposium on Very High Energy Cosmic Ray Interactions Pylos, 6 -12 September 2004 The Modern Concept of the INCA ProjectDirectStudies of Primary protons and nuclei in the “knee” rangeR.A.MukhamedshinInstitute for Nuclear Research, Moscow, Russia for the INCA Collaboration

  2. The INCA Project – Collaboration Members The INCA Collaboration Institute of High-Energy Physics, Protvino, Russia Institute of Ionosphere, Almaty, Kazakhstan Lebedev Physical Institute, Moscow, Russia Institute of Steel and Alloys, Moscow, Russia Abai Almaty State University, Almaty, Kazakhstan Republic Institute for Nuclear Research, Moscow, Russia Institute for Advanced Studies, Tokyo, 162-0022 Japan Institute for Cosmic Research, Almaty, Kazakhstan Republic Institute for Theoretical and Experimental Physics, Moscow, Russia V.V.Ammosov1, V.P.Antonova2, G.I. Britvich1,A.P.Chubenko3, V.I.Drobzhev2, A.D.Erlykin3, G.I. Kol'tsov4, S.V. Kryukov2, G.I. Merzon3, K.K. Mukashev5, R.A.Mukhamedshin6, V.N.Murashev4, V.P. Pavlyuchenko3, V.A.Ryabov3, O.G.Ryazhskaya6, T. Saito7, A.L.Shchepetov3, N.M.Sobolevskii6, A.P. Soldatov1, V.M. Sultangazin8, I.S.Trostin9, G.T.Zatsepin6, A.P.Zhukov6

  3. The INCA Project- Introduction The “knee” problem • is very important forastrophysicsand, may be,physics ofstrong interactions • no unambiguious conclusion onCR spectrum, composition, and, may be,physics • no directmeasurementsat E0> 1015 eV • heavy-material calorimetersareunusabledue to • small acceptanceSW (  0.3 m2sr for Protons); • intense back current To solve the “knee” problem, • large acceptance ( » 1m2sr) • long-duration exposure ( > 1year ) • new approachto energy measurements are required for calorimetric technique

  4. The INCA Project- Objectives Main Scientific Objectives • The spectum& compositionof primary cosmic radiation in the"knee"range (E0 ~ 1015 – 1016 eV); • spectrumof primaryelectrons at E0 ~ 1012 - 1013 eV; • neutrons&g-raysfrom solar flares; • diffusiveg-radiationat E0 ~ 0.010 - 1 TeV; • by-product searches for • verymassive exotic particles with abnormally lowcharge-to-mass ratio (strangelets ?); • interactions with abnormally high hadron-to-g-ray ratio (“Centauros” ?)

  5. The INCA Project- Potentialities Expected number of events detected during 2-3-year exposition : • Number ofprimary nuclei • N(E0 >1015eV) ~ 2000 - 6000 events; • N(E0 >1016eV) ~     40 -   120 events. • Number ofprimary electrons: • N(E0 >1012eV) = 2000 - 6000 events

  6. The INCA Project- Theoretical foundations Main ideas • light-substanceIonization-Neutron CAlorimeter • measurement of theenergyof primary nuclei bytwo independent techniques with: • counting mode forthe thermalized-neutronyield; • amplitude measuring mode for theionization signal • development and use of newest high-tech detector technologies • selection of primary electrons against the protons bycounting neutrons

  7. The INCA Project- Satellite • Dimensions= 2 x 2 x 2 m3 • 4p geometry • Four-dimension cascade picture (x,y,z,t) • SW=48 m2sr • Weight= 10 t • Thickness • 4.6 lint (at E0~1015 eV) • 13 radiation lengths • 50 layers • Number of channels • 40 per layer • 2000 in total

  8. The INCA Project- The INCA satellite project • semiconductor charge detector • Plastic scintillator+leadfor g-ray selection

  9. The INCA Project- Detectors Plastic scintillators • newly developed (IHEP, Protvino) and enriched by orthocarborane(2-3%) to detect thermalized neutrons; • Used to measure both the neutron and ionization signals; • Reactions used for neutron counting: • n + 10B 4a + 7Li* (94%): 7Li + g • Additionally measuredyield of delayedg-rays • n + p d+ g (2.2 MeV) • n + Feg + . . . A part of these • n + Cdg + . . . reactions • n + Gdg + . . .

  10. The INCA Project- Detectors Reactions under consideration: n + 10B 4a + 7Li*7Li + g g from neutron source ionization bya a) Experimental data on neutron detection by a version of scintillation detectors; b) sketch of amplitudes of signals of different origin

  11. The INCA Project- Theoretical foundations- Simulations Energy measurement by evaporated-neutron signal • Yield of neutrons is proportional to the primary energy • Energy dependence of neutron yield is near linearup to energies of the “knee” range • Neutron yield at “knee” energies is ~ 106and long-term (> 100 ms)

  12. The INCA Project- Theoretical foundations- Simulations Fluctuations of neutron yield • Standard deviation ofneutron yieldat effective depth ~250 g/cm2is • ~ 0,30inproton-induced cascades • < 0,25innucleus-induced cascades • Standard deviation incharged-particle flowis of the same order

  13. The INCA Project- Detectors Photo detectors • vacuum phototriodes • newly developedplastic photo-sensitive plates; • PMTs to detect single-neutron capture in plastic scintillators Requirements • wide dynamical range (~ 107); • threshold sensitivity is about 20 MIPs (sufficient at E0>1015 eV)

  14. The INCA Project- Detectors Semiconductor counters • New high-tech detectors of future generation • new-concept pixel silicon detectors with a high space-time resolution are designed • local-injection mechanism for the amplification by bipolar-transistor structure of the drift component of the ionization current produced by relativistic charged particle is exploited

  15. The INCA Project- Detectors • different combination of pixels to reach required properties of the detectors.

  16. The INCA Project- Detectors • Step-by-step transfer of non-basic current carriers along the transistor-cell chain occurs; • matrix-structure detector containing a large number of cells (n-p-n transistors) deposited on a silicon substrate is applied; • DNA molecule-like cell-doubling principle is realized in the matrix structure

  17. The INCA Project- Detectors Experimental samples of new-concept pixel silicon bipolardetectors The use of new-concept pixel silicon bipolar detectors as photodetectors is analyzed

  18. The INCA Project Summary • A high-technology project with unique scientific objectives and potentialities is under elaboration • A new effective technique for direct investigations of the PCR spectrum in the "knee" range atE0> 1015 eV is developed. • A state-of-the-art technologyfor investigation of primary cosmic radiation is under elaboration The INCA Project is open for the international community!Collaborators are welcome!

  19. Thank you!

  20. The INCA Project – Main Guidelines and Problems of INCA Design Stage 1. Design and testing of technological elements • Scintillators • Phototriodes • Plastic photo-sensitive plates • Pixel silicon bipolar transistor detectors • Simulations

  21. The INCA Project – Main Guidelines and Problems of INCA Design Stage 2. Construction of apparatus modules • Main Calorimeter • Charge detectors • Reading and processing systems • Electronics • Data processing algorithms Stage 3. Testing of apparatus modules • Accelerator experiments

  22. The INCA Project – Collaboration Possible directions of collaboration • Production of pixel silicon bipolar transistor detectors • Development of reading and processing systems • Development of electronics • Construction and launching of joint balloon equipment for • Testing the systems • Study of electron primary spectrum at E0 > 1 TeV • Submitting joint applications for financial support of joint investigations into CRDF (Civilian Reseach & Development Foundation), ISTC (International Science & Technology Center), INTAS etc. • Satellite ?

  23. The INCA Project – Technological Elements of INCA Design Scintillators: • already developed • cost: ~ 75 $ /1 kg (or less) • specific configurations can be produced at any time • arbitrary configurations can be produced if a corresponding mold is constructed Stage 1

  24. The INCA Project – Technological Elements of INCA Design Phototriodes: • already developed • cost: ~ 30 $ each • can be produced at any time Plastic photo-sensitive plates • already developed • cost: ~ 1 $ /1 cm2 • can be produced at any time Stage 1

  25. The INCA Project – Technological Elements of INCA Design Pixel silicon bipolar transistor detectors: • the most interesting and promising detectors of the next generation • know-how is patented • developed least of all • cost: ~ 30 - 200 $ /1 dm2 (depends on silicon base purity) • features are strongly dependent on • silicon quality • quality of spatial technology resolution (~ 1 m2 is requiredfor ~102-amplification by one pixel) • it seems that detectors with a very good features cannot be produced in Russia: the most promising direction of a collaboration Stage 1

  26. The INCA Project- Theoretical foundations– Simulations Basic codes • The MC0 code of strong interactions (usable up to ~1018 eV) and package SHIELD are used for simulations • The MC0 code is based on: • data by accelerator experiments • Quark-Gluon String model by Yu.Shabelsky • Semi-hard jet theory by Gribov-Levin-Ryskin • The MC0 code describes rather well • accelerator data • data ong-h families observed in X-ray emulsion chamber experiments • The neutron-transportpackage SHIELDis : • based on data by accelerator and neutron experiments • specially designed for neutron investigations Stage 1

  27. The INCA Project- Theoretical foundations- Simulations The QGSM-based MC0 code (close to QGSJET) realizes • Hadron interactions as • soft hadron interactions • semi-hard and hard jet generation • diffraction processes • generation of stable and resonance baryons and mesons, including charm and strange particles • Electromagnetic cascadewith accounting for • pair generation • bremsstrahlung • multiple Coulomb scattering • Compton scattering • ionization losses • inelastic photonuclear interactions of g-rays • LPM effect at high energies • giant resonance absorption of low-energy g-rays Stage 1

  28. The INCA Project- Theoretical foundations- Simulations TheMC0code realizes generation of neutrons as • neutron evaporationby nuclei excited due to • hadron interactions • inelastic photonuclear interactions of g-rays; • absorption of low-energy photons in giant resonance processes; • neutron generationin hadron cascade interactions Stage 1

  29. The INCA Project- Theoretical foundations- Simulations Notes: • Only the neutron generation is mainly considered, not neutronhistory • Such factors as • neutron thermalization and diffusion • real geometry • apparatus response • role of the primary spectrum will be carried out in the nearest future Stage 1

  30. The INCA Project- Theoretical foundations- Simulations Prototype simulations • a setup 500-g/cm2 thick (~7lint) with a periodic structure is considered • each of layers consists of lead and a light substance (polyethylene, e.g.) • lead layer: 10 g/cm2 (~1.5 rad. length, ~1/20lint) • polyethylene layer: 20 g/cm2 (~0.5 rad. length, ~1/4lint) Stage 1

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