PowerPoint 2
Neutrino is a lepton, first proposed by Pauli to explain the conservation during decay.
The extremely small cross section of neutrino lead to a tough detection. Neutrino was first detected in 1957 by capture, proposed by Wang Ganchangin 1942.
Neutrino Basics 3
The observed flux of neutrino is only 1/3 of the expectation. Neutrino oscillation was found and 3 flavors of neutrino have been proved.
Mixing angle and the mass is the key to a better understanding of neutrino oscillation.
Neutrino Basics
real-time information such as
SNe …
Neutrino Basics
Why Neutrino?
5
Different energy regime of neutrino helps to understand the different model better.
Sun 0.1 MeV – 1MeV
SNR neutrinos – 30 MeV
GZK cut-off – 1EeV
Cosmic rays > 1019.5 eV from 50 Mpc should not be detectable.
Solar: 6 × 1010 /(cm2 s) Cosmic neutrino
background : 6 × 1010/cm3
SNR GZK cutoff
6 Neutrino Basics
Water detector Cherenkov photons
Ice cube
Neutrino Detection 7
Liquid scintillator detector
Askaryan Radiation (1962) A particle traveling faster than
the phase velocity of light in a dense dielectric produces a shower of secondary charged particles which contain a charge anisotropy.
Strong radio-frequency (RF) emissions from high energy will be radiated as showers in dielectric media.
Air & Ice & Salt rock & lunar regolith
Radio wave generated by the electron shower during the propagation of the particle
9 Neutrino Detection
Radio Wave Radiation
Spectrum and phase simulation by different models of Askaryan radiation.
10 Neutrino Detection
Radio Wave Radiation
Askaryan Radiation Spectrum
under 100 – 300 m
• Half-wave dipole antenna(400 MHz)
• AGNs, GRBs, Monopole decays,
Half-wave antennas
• 104 km3 sr
• Attenuation length ~1km
• 1018 eV (GZK cut-off)
The coverage of one
• Synaptic lightning observation
• Greenland ice (1997-1999)
• 19 million km3
neutrino
• Aim at neutrinos > 100EeV
• 2 antenna at Goldstone
• loss tangent with an average tanδ = 0.003,
• Attenuation length ~ 9m at 2Ghz
• 600 km3 sr
16 Neutrino Detection
17 Neutrino Detection
CJPL
China JinPing Laboratory (CJPL) 18
The muon flux and the reactor neutrino flux of different experiments and the red one is Jinping who has least indicating Jinping has the best resolution.
CJPL is under an overburden of over 2000 m to reach a least background.
19 China JinPing Laboratory (CJPL)
China JinPing underground Laboratory (CJPL)
Department of Engineering Physics, Tsinghua University
Center for High Energy Physics, Tsinghua University
20 China JinPing Laboratory (CJPL)
Jinping Neutrino Experiment
Possible muon incident direction
Motivation
~3km
~3km
23
=
( − 1)
Software Defined Radio
Software defined radio (SDR) process the radio signal by software. The signals are received directly and carry out more information. One can get what he wants freely.
25 Tsinghua Open Low-frequency Array (TOLA)
RTL-SDR
be used as a computer based
radio scanner for receiving live radio signals in your area (no
internet required).
Bandwidth from 100KHz to 1706 MHz
Sampling rate Up to 3.2 MSa/s. But only stable under 2.4M/s
Sample resolution 8 bits, with effective number estimated at around 7
Amplifier +26dB proveided by LNA, and +15dB provided by VGA
Energy Cost around 2.5 W
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Low-cost, high-performance computers that people use to learn, solve problems and have fun.
Low Energy Use.
Pre-process data and Upload data.
~9cm
~6.5cm
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28
TOLA-V0.1
Two monopole antennas interferometry
… SDR
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TOLA-V0.1
System Calibration : LO Shift
System Calibration : Clock Error
6~16 Antennas (Dipole)
Conclusion
astronomy and physics.
low frequency band.