New design of an acoustic array calibrator for underwater neutrino - - PowerPoint PPT Presentation
2 nd International Electronic Conference on Sensors and Applications 15-30 November 2015 New design of an acoustic array calibrator for underwater neutrino telescopes M. Saldaa, C.D. Llorens, I.Felis, J. A. Martnez-Mora and M. Ardid UPV
2nd International Electronic Conference on Sensors and Applications 15-30 November 2015
UPV – IGIC – Campus de Gandia (València)
New design of an acoustic array calibrator for underwater neutrino telescopes
New design of an acoustic array calibrator for underwater neutrino telescopes G.A.Askaryan. Hydrodynamical emission of tracks of
ionising particles in stable liquids. J. At. Energy 3 (1957) 921.
2
dt d 2
Temperature Time
𝒊 ∝ 𝜷 𝜸 𝑫𝒒
h ∆t
The Thermo-Acoustic Model
Energy deposition when a neutrino interacts with nuclei in water
Neutrino Telescope Deep Sea
Induces a local heating in a very short period of time leading to a short pressure pulse signal
A good acoustic calibrator can be very important to study the feasibility of the UHE neutrino acoustic detection technique and help to discriminate the signal from noise and background of transient signals. Useful tool to:
Campaigns or integrated in the infrastructure).
New design of an acoustic array calibrator for underwater neutrino telescopes
a non linear effect used in different underwater applications.
beams from 2 directive high-frequency beams
modulation
high-frequency signal will be absorbed.
usually less than 1%
Primary f1=418 kHz Primary f2=482 kHz Secondary f2-f1=64 kHz
New design of an acoustic array calibrator for underwater neutrino telescopes
Neutrino-like signals generation is achieved by using parametric acoustic sources
New proposed design composed of an array of piezo ceramic tube transducers array emitting in axial direction
Processes involved in the design
Array composed of new piezo tube ceramics emitting in axial direction Operation at high-frequency by the parametric technique New specific electronics adapted to the transducers
New design of an acoustic array calibrator for underwater neutrino telescopes
Receiver RESON TC4038
Two Piezo-Tube Ceramics under study
Receiver Emitter
Water Tank Amplifier NI PXI 1031 DC - LAbView
Equipment for characterization
System Characterization at the Laboratory water tank
UCE-534541 OD=5.3 ID=4.5 H=4.1 [cm] UCE-343020 OD=3.4 ID=3 H=2 [cm] [Freq Range 10kHz–1MHz] New design of an acoustic array calibrator for underwater neutrino telescopes
Generator/Acquisitor
Primary frequency of resonance is around 490 kHz and secondary resonance frequency at low frequency around 35 kHz.
Characterization of piezo-ceramics
UCE-534541 OD=5.3 ID=4.5 H=4.1 [cm]
Low frequency High frequency
New design of an acoustic array calibrator for underwater neutrino telescopes
New design of an acoustic array calibrator for underwater neutrino telescopes
10 20 0.2 0.4 0.6 0.8 1 Angle [º] Normalized amplitude Axial Directivity UCE Ceramic
534541 343020
0.8 0.85 0.9 0.95 1 1.05 1.1 1.15 150 155 160 165 Frequency / Resonance Frequency Sensitivity (dB re uPa/V) TVR Ceramic UCE
534541 343020
10 20 30 40 50 60 70 80 90100 130 132 134 136 138 140 142 Frequency (kHz)
Sensitivity (dB re uPa/V @1m)
TVR Ceramic UCE
534541 343020
Characterization of piezo-ceramics
Moulding RoyaPox511 Resin Moulding Poliutherane EL241F
First Tests for Ceramic Moulding (Heading/Backing)
No Loses 4-5 dB Loses
Next To Study the Effect on Parametric Emission
New design of an acoustic array calibrator for underwater neutrino telescopes
Goal
Thickness matching accomplish λ/4
ceramic resonance frequency
New design of an acoustic array calibrator for underwater neutrino telescopes
First Studies of the Parametric Bipolar Pulse Emission
Original Received Signal (blue) and Filtered Received Signal (red) at low-frequency [5 kHz - 80 kHz]
Bipolar Shape
The viability of the technique has been checked
0.7 0.72 0.74
2
Received Signal Time(ms) Amplitude(V)
Original Filtered(x20)
0.2 0.4 0.6 0.8 1 0.5 1
Amplitude Input Signal(V) Normalized Amplitude Received Signal
Original Filtered
Non-Linearity
2 4 6 0.2 0.4 0.6 0.8 1
Angle [º] Normalized amplitude Directivity Horizontal
Non-Filtered Filtered
Similar Directivity
Low Frequency: Emitting long non directive signals Easy to detect High Frequency: Emitting long parametric directive signals HF: Parametric Bipolar signal: transient & directive 1st Stage 2nd Stage 3rd Stage TAGGING the BIPOLAR pulse emissions Calibration in 3 Steps, increasing difficulty Challenge: Detecting the High directivity Bipolar pulse emitted from several km away
Three Operation Modes
New design of an acoustic array calibrator for underwater neutrino telescopes
Functionalities: Training and tuning the acoustic detector, cross-checking the detector hydrophones
have a good sensitivity in both high and low frequency and narrow beam directivity at the high frequency which will lead to a tight low-frequency (parametric) directivity.
the high frequency emission.
New design of an acoustic array calibrator for underwater neutrino telescopes
New design of an acoustic array calibrator for underwater neutrino telescopes
FPA2012-37528-C02-02, CSD2009-00064, PrometeoII/2014/079, ACOMP/2015/175
Acknowledgements:
New design of an acoustic array calibrator for underwater neutrino telescopes