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Low-Cost Solid-State Cosmic Ray Observatory

Multiple nodes detect photons to within nanoseconds to analyze cosmic ray air showers and help solve the Greisen-Zatsepin-Kuzmin paradox.

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This project was created on 08/13/2014 and last updated 6 days ago.

Description
This is a new design for a cosmic ray observatory consisting of small, low-cost, easy-to-use, internet-connected detector nodes based on PIN diodes. Cosmic rays are particles and nuclei which bombard the earths atmosphere and create cone-shaped showers of secondary particles. Observatory nodes are able to detect and record the time of impact of single gamma ray photons of these showers to within a few nanoseconds, as well as the energy of the photon, and are low-cost enough to create cosmic ray observatories of unprecedented size. Nodes communicate to a central database to upload data, which is later analyzed to determine the energy, angle, and location of the original cosmic rays. This information can be used to learn about the origin of ultrahigh-energy cosmic rays and can help solve the Greisen-Zatsepin-Kuzmin paradox, in which the experimentally determined cosmic ray energies are higher than theoretically possible.
Details

1. BACKGROUND

Cosmic rays are particles and nuclei which bombard the earth from all directions [1]. The Greisen-Zatsepin-Kuzmin (GZK) limit is a theoretical upper limit on the energy of cosmic rays from distant sources of 5*10^19 eV. The limit is set by their propagation to us through the cosmic microwave background radiation (CMBR) [4]. However, cosmic ray energies have been experimentally determined to vary from 10^8 eV to well beyond 10^20 eV. The identification of sources of ultrahigh-energy cosmic rays (UHECR), cosmic rays from distant sources with energies above the GZK limit, has been a great challenge since they were first observed in 1962 [1]. The observed existence of these particles is the GZK paradox: Why is it that some cosmic rays appear to possess energies that are theoretically too high, given that there are no possible near-Earth sources, and that rays from distant sources should have scattered off the cosmic microwave background radiation?

Detecting the cosmic rays themselves is difficult; only a handful have been directly detected in the last 50 years. The only way to detect UHECR is through their interaction with the earths atmosphere, producing a cascade of billions of particles that excite nitrogen molecules in the air and spread out over a large area once they reach the ground [1]. When a primary cosmic ray produces many secondary particles, this is called an air shower. When many thousand, millions, even billions of particles arrive at ground level this is called an extensive air shower (EAS). When cosmic rays interact with nuclei in the air, pi-mesons (pions) are created. Neutral pions decay very quickly, usually into two gamma rays. The gamma rays from the neutral pions may also create new particles, an electron and a positron, by the pair creation process, and these electrons and positrons may produce more gamma rays by the bremsstrahlung mechanism. Charged pions decay into a muon and neutrino but after a longer time than neutral pions, so some charged pions may collide with more nuclei in the air to produce even more new particles [2].

These air showers form cones of particles, meaning detectors on the ground can determine the place in the atmosphere where the original cosmic ray hit. Dozens of such cosmic ray observatories exist. In 2007, the Pierre Auger Observatory, consisting of 1600 detectors spaced 1.5km apart, found a strong association between cosmic ray direction and nearby active galactic nuclei, galaxies hosting central black holes which may eject plasma jets into intergalactic space [1]. However, more observatory data are necessary to properly understand cosmic rays and solve the GZK paradox. 

2. DESIGN

Figure 1: Flow of information within each observatory node

The cosmic ray observatory is comprised of many individual detector nodes. When struck by a single gamma ray photon, a node must be able to record the time the photon struck to within a few nanoseconds, the energy of the photon, and the location of the node. It must then be able to store this data and later send it to a master database. Each node contains two microcontrollers: a timing microcontroller dedicated to precisely measuring the time the photon strikes, and a logging and interface microcontroller to measure photon energy, record data to an SD card, and communicate with the master server. Both can be atmel atmega microcontrollers, and the logging and interface microcontroller can be a raspberry pi. However, the timing microcontroller cannot be a raspberry pi because even with a real-time linux kernel, latency is inconsistent and unacceptably high at around 28 microseconds [3].

Figure 2: PIN diode gamma ray photo detector. Current generated when a photon strikes the PIN diode is amplified through four op amps; a comparator then sends a pulse when the signal dips below a threshold. 

The heart of a node is its PIN diode detector (figure 2), based on a 2003 Maxim application note, which uses a photodiode...

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Project logs
  • What to detect

    16 days ago • 1 comment

    I've been doing a bit of reading on other solid state detectors and have decided that it's a great idea to detect muons rather than gamma rays. Secondary showers consist mainly of electrons, photons, and muons. Unlike photons, muons are easily able to pass through thick metal shielding. This means I can detect only muons by adding thick metal around the pin diode. (I was going to add some shielding anyway to prevent electromagnetic interference. I realize now that this simultaneously decreases gamma ray sensitivity in a somewhat unpredictable way.) The benefit of detecting muons rather than gamma rays is that the node will detect less terrestrial background radiation, which is important if I intend for the node to be used in somewhat populated areas.

    At this point I'm not sure what kind of material or thickness is needed for the shield, nor am I totally positive that detecting only muons is the right way to go. Thankfully, my detector design is flexible enough that I can continue working on the electronics and software while simultaneously working on the particle physics aspect.

    Coincidence detection might also be something to look into. This is where two PIN diodes (or hopefully array of diode) have shielding in between them, and a circuit is used to record only events where the top detector get a pulse a certain amount of time before the bottom detector. This should reduce terrestrial radiation interference even more.

  • Hooray!

    21 days ago • 0 comments

    I made it to the top 50! I just need to make sure I keep working on and documenting this project.

  • Future Goals

    a month ago • 0 comments

    Right now I’m assembling a first prototype of the detector node. I’ve determined a few things which need to get done in order to make sure the device will work how I’d like it to.

    1. Optimize timing accuracy

    I’d first like to see how I can modify the GPS settings to get the most accurate clock pulses. I also want to experiment to find the best algorithm for utilizing the GPS pulses. This means measuring how many Arduino clock pulses it takes for a single GPS pulse over time, and seeing if averaging is necessary. This also means making more intelligent code which accommodates for the timer ticking while each byte is recorded. (I haven't thought through that last part entirely, but I may not have to accommodate for this delay as long as it is consistent.)

    2. Optimize protocol for server communication

    I need to find a balance between minimal processing by the Arduino and minimal transmission size. I also need to determine if the detector node should immediately send data, or rather accumulate data on the SD card and then send it to the server.

    3. Increase detector sensitivity

    I realize now that a single pin diode probably isn’t enough. This means I need an array of pin diodes. I need to determine which pin diode on the market is most worth its cost. I also need to determine which amplification circuits and ICs work the best.

    4. Determine calibration procedure

    All nodes need to have the same sensitivity and delay; this means calibration is important. I need to determine where in the circuit pots or adjustable caps are required, and what accuracy each discreet component needs to be. Then, I need to find a good way to ensure that the nodes can be calibrated without any expensive test equipment. One idea I have is to use readily available americium from smoke detectors to calibrate sensitivity.

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Discussions

Felipe Muniz wrote 4 days ago null point

A geiger tube isn't useful? Some tubes are very cheap, check on Ebay.

I also remember of this projects here, one use photodiode and other use a webcam to detect radiation.

http://www.vk2zay.net/article/265
http://www.inventgeek.com/alpha-radiation-visualizer/

Are you sure? [yes] / [no]

Jan-willem De Bleser wrote 5 days ago null point

Fantastic idea! The more data we have, the better, so a distributed detector would be excellent.

Have you started thinking about the data collection infrastructure yet? Anyone who wants to do some of the calculations you're talking about will need more than just their own dataset, so you'll need some way of distributing or gathering all the individual measurements. Do you envision running a central repository somewhere, where the RPIs can upload and scientists can download? Or what about something distributed, say RPIs in a p2p network distributing all measurements to all (interested) nodes?

I'd be interested in building one myself, and tinkering with the design.

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aelias36 wrote 4 days ago null point

Hi there,
I have't put to much thought into networking just yet. As another commented posted below, I would probably like to look at Blitzortung, which has a similar setup but with detecting lightning. Thanks for the p2p idea; that sounds promising.

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Jonr.westfield wrote 5 days ago null point

Great project!

Have you got any more documentation yet?

Thanks :D

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aelias36 wrote 5 days ago null point

I was very busy with school this past week, but more documentation is sure to come! I recently spoke with an astrophysicist who researched and wrote his dissertation on cosmic rays and their detection, and I'll be writing about what we discussed soon.

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masoud wrote 19 days ago null point

Very interesting project and congratulations for being selected. I am happy to see many scientific projects selected.

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Legionlabs wrote 21 days ago null point

I used the Hamamatsu Photonics S1223-01 photodiode to detect 20MeV alpha particles with an almost identical op-amp chain. It worked really well, but was expensive and difficult to source. The first opamp stage required a full Faraday cage.

I tested many other PIN photodiodes without luck, but I'm confident a cheaper and more available option exists. The most promising avenue was a design I saw somewhere that used solar panels as a cheap detector in a small particle accelerator, as they are essentially high surface area PIN photodiodes. I never got it working.

I have read rumors that the venerable 2N3055 power transistor can be decapped and works, but cannot confirm.

I can share notes if useful to you.

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PointyOintment wrote a month ago null point

Do you know about Blitzortung? It basically does the same thing for lightning, so it might be good to look at their electronics and algorithms.

http://www.blitzortung.org/

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aelias36 wrote a month ago null point

I did not. Thanks for the link!

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aelias36 wrote a month ago null point

I recently learned about something very interesting: some scientists propose almost all lighting is triggered by cosmic rays. This means comparing data between lighting and cosmic ray detectors could be very useful. Again, thanks for the link!

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