Must be done a premise, the detectors described in the previous page, want to be emotional objects, in fact, are one of the few methods that can make us "see" elementary particles otherwise detectable only by specific instruments, and are a great vehicle to introduce the subject of cosmic Astroparticles at any level of divulgence.
The instrument described here is a direct evolution of the previous and is able to count muons but does not want to have some claim to be a perfect or very accurate, if you need a measuring instrument, there are other ways to follow. What has been tried and wanted to do is to keep the visual aspect combined with the emotional-feeling instrument and the goal was achieved.
This implementation maintains the characteristic of being reproducible at low cost, unlike the others, however, the work of implementation is very tough so it is recommended only for those who have experience of manual work and good knowledge of electronics.
Principle of operation:
The heart of the system is composed of three common fluorescent circular tubes, divided at 120° into three sectors, a hyperbolic mirror collects light of the lamps that is reflected by the secondary mirror like in a standard Newtonian telescope.
The sensor is then composed of nine sectors in groups of three detectors, the diagram below best explains operation:
What appears to be looking into the eyepiece is visible in the animation, unlike other detectors which must be keept in complete darkness, this can be observed even in ambient light (better still obscure) because the pipes are enclosed into a dark room.
The brain of the detector was a real technical challenge to the boundaries between classical physics and quantum physics and even more interesting.
Suffice it to say that the impedance of the frames is several giga-ohms and the current to be detected is a few hundred nano-amperes. How do we teach the Heisenberg microscope, any attempt to measure impact on the experiment by making a change in behavior and sometimes stop working!
Ultimately, it was however found a safe and reliable system for tracking number.
When a muon passes through the detector at an angle not exceeding 12°, all the tubes are interested and will light on at least three areas, if the angle of incidence is between twelve and 27° light up the areas of two adjacent tubes, for upper angles of incidence only one tube will be affected, and then lights on.
For counting is considered as one muon at least two areas of coincident turn on of two adjacent tubes, (a field for each tube) but the instrument can be set to record any pulse received on any field.
A simple electronic counter records the pulses and an audio output is connected to a computer for counting and possible timing diagrams, there is indeed a very good freeware software, build for geiger counters, that fits perfectly this instrument.
It 'was then set up a serial RS232 for future development of a dedicated hypothetical software.
For high voltage have been found other low-cost solutions, such as power supplies for lamps (CCFL in LCD laptop) or the shoe-killing mosquitoes with the appropriate changes, but in the end are yet been used the circuits for the flash-lamps for the characteristic of being extremely stable and keeping the output voltage value constant regardless of the state of battery charge.
Three sensitive photodiodes capture the low light flashes that generate the muons by means of an ingenious contrivance, in fact the neon flashing are so weak that only expensive avalanche diodes or photomultipliers could perceive. Other systems of measurement are recognized ineffective or invasive or they lose the sense of emotional detector mentioned above.
The logic of the detector is mounted on a breadboard and inserted into the top of the telescope tube with the high-voltage circuit and battery power.
Testing and operation:
Below test on the operation of the sensor of the telescope:
Video regarding the operation, the software records the events:
At the first start, after exactly one hour, the counter of the instrument signals 563 muons on a surface area of approximately 18cm2 with the coincident method, means muons 99% on average perfectly with that measured almost anywhere in the world, 'about' at sea level (here we are at 390mt.). Software metering gives us an average of 540 cph.
The software used is the simple as complete cdv counter written by David Honig, producing recordings of readings and graphs, as well as, contains a web server, you can then plug in the network and produce real-time detection available on the web! This could be a future development on the site astroparticelle.it, we'll see ...
One limitation of the software is that since it was created for a specific tool, depending on the threshold value plays a single pulse as more pulses, so every time you must make an adjustment, in the examples shown the recorded data have been reinterpreted by dividing the correction factor (8), those exposures in the graph are the actual values.
|Set A (any flash)|
|Set μ (coincident flashes)|
From other measurements, the values are between 900 (A) to 440 (μ) on average, there is no real reasons to believe that the instrument not register only muons, but the setting μ "filters" so to speak signals impure, but certainly also filters muons with angles of incidence that involving only one sensor.
Average/h Set "A" = 942
Average/h Set "µ" = 440
Limitations and problems:
The operating limits encountered time to time will be inserted here:
Some phases of construction:
mounting fluorescent tubes.
first 'sensor' tests
The counter after almost an hour of operation from the first test.
AMD3 Astroparticle μ detector-counter ver. III
-Method: Ionizing gas
- Sensor: 3 Neon tubes with 3 frames
- HV=1272 V d.c.
- S□≈51 cm2
- Detection1: [μ] Coincident ≈27°max.(2 closer tubes any frames)
- Detection2: [A] Any (any tube any frame)
- Output: 2x audio signal - 1x rs232
- Power source: 4x 1,5V. AA - 1 x 9V. E/6LR61.
Pevatron all'interno della nostra Galassia 9.04.2021
L'osservatorio per raggi gamma in Tibet ASγ ha osservato nel disco galattico 23 raggi gamma diffusi ad altissima energia - tra 100 TeV e 1 PeV. In particolare, tutti i raggi gamma superiori a 398 TeV sono stati osservati separatamente dalle sorgenti di raggi gamma TeV note e compatibili con le aspettative dallo scenario di emissione adronica, in cui i raggi gamma hanno origine dal decadimento di pioni neutri prodotti dall'interazione dei protoni primari con il mezzo interstellare nella Galassia. Questa è una forte prova che i raggi cosmici sono accelerati oltre le energie PeV (1015 eV) all'interno della Galassia e si diffondono nel disco galattico.
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