INCA13ISVHECRI

The Modern Concept of the INCA Project Direct Studies of Primary protons and nuclei in the “knee” rangeR.A. Mukhamedshin Institute for Nuclear Research, Moscow, Russia for the INCA Collaboration: 

The Modern Concept of the INCA Project Direct Studies of Primary protons and nuclei in the “knee” range R.A. Mukhamedshin Institute for Nuclear Research, Moscow, Russia for the INCA Collaboration XIII International Symposium on Very High Energy Cosmic Ray Interactions Pylos, 6 -12 September 2004

The INCA Collaboration: 

The INCA Collaboration 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 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 The INCA Project – Collaboration Members

The INCA Project - Introduction: 

The INCA Project - Introduction The “knee” problem is very important for astrophysics and, may be, physics of strong interactions no unambiguious conclusion on CR spectrum, composition, and, may be, physics no direct measurements at E0> 1015 eV heavy-material calorimeters are unusable due to small acceptance SW (  0.3 m2sr for Protons); intense back current To solve the “knee” problem, large acceptance ( » 1 m2sr) long-duration exposure ( > 1 year ) new approach to energy measurements are required for calorimetric technique

The INCA Project - Objectives: 

The INCA Project - Objectives Main Scientific Objectives The spectum & composition of primary cosmic radiation in the "knee" range (E0 ~ 1015 – 1016 eV); spectrum of primary electrons at E0 ~ 1012 - 1013 eV; neutrons & g-rays from solar flares; diffusive g-radiation at E0 ~ 0.010 - 1 TeV; by-product searches for very massive exotic particles with abnormally low charge-to-mass ratio (strangelets ?); interactions with abnormally high hadron-to-g-ray ratio (“Centauros” ?)

The INCA Project - Potentialities: 

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

The INCA Project - Theoretical foundations: 

Main ideas light-substance Ionization-Neutron CAlorimeter measurement of the energy of primary nuclei by two independent techniques with: counting mode for the thermalized-neutron yield; amplitude measuring mode for the ionization signal development and use of newest high-tech detector technologies selection of primary electrons against the protons by counting neutrons The INCA Project - Theoretical foundations

The INCA Project - Satellite: 

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 l int (at E0~1015 eV) 13 radiation lengths 50 layers Number of channels 40 per layer 2000 in total

The INCA Project - The INCA satellite project : 

The INCA Project - The INCA satellite project semiconductor charge detector Plastic scintillator+lead for g-ray selection

The INCA Project - Detectors: 

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 measured yield of delayed g-rays n + p  d + g (2.2 MeV) n + Fe  g + . . . A part of these n + Cd  g + . . . reactions n + Gd  g + . . .

The INCA Project - Detectors: 

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

The INCA Project - Theoretical foundations - Simulations: 

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 linear up to energies of the “knee” range Neutron yield at “knee” energies is ~ 106 and long-term (> 100 ms)

The INCA Project - Theoretical foundations - Simulations: 

The INCA Project - Theoretical foundations - Simulations Fluctuations of neutron yield Standard deviation of neutron yield at effective depth ~250 g/cm2 is ~ 0,30 in proton-induced cascades < 0,25 in nucleus-induced cascades Standard deviation in charged-particle flow is of the same order

The INCA Project - Detectors: 

The INCA Project - Detectors Photo detectors vacuum phototriodes newly developed plastic 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)

The INCA Project - Detectors: 

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

The INCA Project - Detectors: 

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

The INCA Project - Detectors: 

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

The INCA Project - Detectors: 

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

The INCA Project: 

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 at E0 > 1015 eV is developed. A state-of-the-art technology for investigation of primary cosmic radiation is under elaboration The INCA Project is open for the international community! Collaborators are welcome!

Slide19: 

Thank you!

The INCA Project – Main Guidelines and Problems of INCA Design : 

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

The INCA Project – Main Guidelines and Problems of INCA Design : 

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

The INCA Project – Collaboration: 

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 ?

The INCA Project – Technological Elements of INCA Design : 

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

The INCA Project – Technological Elements of INCA Design : 

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

The INCA Project – Technological Elements of INCA Design : 

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 required for ~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

The INCA Project - Theoretical foundations – Simulations: 

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 on g-h families observed in X-ray emulsion chamber experiments The neutron-transport package SHIELD is : based on data by accelerator and neutron experiments specially designed for neutron investigations Stage 1

The INCA Project - Theoretical foundations - Simulations: 

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 cascade with 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

The INCA Project - Theoretical foundations - Simulations: 

The INCA Project - Theoretical foundations - Simulations The MC0 code realizes generation of neutrons as neutron evaporation by nuclei excited due to hadron interactions inelastic photonuclear interactions of g-rays; absorption of low-energy photons in giant resonance processes; neutron generation in hadron cascade interactions Stage 1

The INCA Project - Theoretical foundations - Simulations: 

The INCA Project - Theoretical foundations - Simulations Notes: Only the neutron generation is mainly considered, not neutron history 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

The INCA Project - Theoretical foundations - Simulations: 

The INCA Project - Theoretical foundations - Simulations Prototype simulations a setup 500-g/cm2 thick (~7 lint ) 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, ~1/20 lint ) polyethylene layer: 20 g/cm2 (~0.5 rad. length, ~1/4 lint ) Stage 1