University of Kansas QuarkNet Center
Submitted by Anonymous (not verified)
on Tuesday, June 4, 2013 - 21:22
Description
A collaboration of teachers, students and physicists involved in inquiry-based, particle physics explorations.
Commissioning a Cosmic Ray Muon Detector for Cosmic Ray Radio Wave Research
Names: Brittany Crossen, Ottawa High School, Ottawa, KS
Ardrian Tidwell, Insight School of Kansas, Olathe, KS
Research Teacher Mentor: James Deane, Ottawa High School, Ottawa, KS
Research Mentor: Prof. Dave Besson, University of Kansas, Lawrence, KS
Purpose: We are building apparatus to help us detect and characterize radio wave emission from cosmic ray impacts in the upper atmosphere and the particle showers they create. As part of this we learned how to use and operate a Cosmic Ray (Muon) Detector, or CR(M)D, for the purpose of detecting and analyzing showers produced by cosmic rays. The ultimate goal is to find the correlation between cosmic ray showers and cosmic ray generated radio waves. It is important to ensure that our system only triggers on events that are extremely likely to be muons from cosmic ray showers, and that the trigger rate is compatible with the radio digitization hardware.
Methods: we began with a partially assembled CRMD. Several issues were discovered, including a PMT which did not operate at the same frequency as the others at the same tube supply voltage. We were able to calibrate this tube at a higher voltage, and it seems to operate and gives expected results compared to the other tubes. We also spent some time familiarizing ourselves with the computer commands necessary to communicate with and control the various settings of the Digital Acquisition board (DAQ). However, the commands and language were eventually deciphered and new avenues of data acquisition were opened.
Several pieces of hardware were used jointly to achieve data collection, from the QuarkNet Data Acquisition Board (DAQ) to the individual detectors. We used Ubuntu linux and the SCREEN program to connect, control, and collect data from the DAQ. Some of the commands for changing settings on the detector were discovered in the process of troubleshooting.
Results: We have evaluated multiple paddle configurations and settings to properly trigger the radio receiver and radio data acquisition part of the experiment. However, further testing is needed to evaluate more configuations and determine optimal settings. For this reason, more data in different scintillator paddle configurations is being collected and analyzed to reduce the trigger rate to a frequency where the radio wave detector and acquisition system can operate (around 50 triggers per second).
We are adjusting the following variables: coincidence number, gate width (the time window during which the detectors need to be activated, starting from the first detector’s activation), threshold level (the “strength” of the signal from a detector), and the geometry of the detector paddles.
The project is still incomplete, as the best detection rate we have so far achieved has not met the goal detection rate. We also need to determine how well we are discriminating true cosmic ray shower events. Comparing our count rate at the paddle and DAQ configurations we have used, we think there may still be false detector signals.
Meaning to Larger Project: The CRMD is intended to be used with a radio wave detector and digitizing system. The CRMD will detect cosmic rays by their muon showers and create a focus period for the radio wave detector. Studying radio wave emissions may give us further insight into the origin and characteristics of the particles that are cosmic rays.
Future Research:
Continuing to adjust the settings and geometry of the detector to increase the discrimination and decrease trigger rate is necessary to be able to continue to the final goal of radio detection. The radio wave detector, antenna, and digitizer will need to be added to the experimental setup and calibrated. The CRMD triggering will signal the digitizer to trigger and potentially capture cosmic ray radio signals, the original and ultimate goal of the project.
Acknowledgements:
We would like to thank the following for their assistance during the course of this research:
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Josh Macy, Undergraduate, University of Kansas, Lawrence, KS
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Dave Hoppert, Fermilab, Batavia, IL
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Mark Adams, Fermilab, Batavia, IL
Further Development of Lightning Detection and Triggering for the TARA Experiment (2016)
Names: Bennett Haase-Divine, Lawrence Freestate High School
Pierce Giffin, Shawnee Mission East High School
Research Teacher Mentor: James Deane, Ottawa High School, Ottawa, KS
Research Mentor: Prof. Dave Besson, University of Kansas, Lawrence, KS
Purpose: The purpose of our project was to accurately detect flashes of lightning as well as determining their approximate position and time of strike so that other devices involved in the TARA project can study and collect data from flashes of lightning while they’re still striking. This research continues and extends research from previous years.
Methods: For light detection, we used several photoresistors and an arduino board that read the voltage off of each resistor. The program constantly averages out all reading over a brief period of time. If a single reading spikes up above this average, the program would identify it as a lightning strike. As soon as a flash of lightning is detected, a signal is sent out to alert other devices that lightning has struck. To calculate the angle the strike occurred relative to the device, we see how high the voltages are on each photoresistor relative to one another and weight each voltage with the photoresistor’s assigned angle. After all the data is collected, it is stored on a micro SD card inside of the device with an absolute time stamp from a GPS chip.
Results: Almost all of the necessary operations work properly with a simulated strobe machine. The device is capable of detecting nearly 100% of simulated flashes and calculating the correct angle within about 4o. The signal is capable of being sent out to other devices within 5 milliseconds. The device can accurately identify two flashes of lightning within 20 milliseconds of each other. Since a single lightning strike flashes once then flashes again about 30 milliseconds later (and can repeat several more times), the device is capable of detecting a strike of lightning on the first flash then sending out a signal to other devices to collect data on other flashes. With recent testing we believe our device can detect lightning up to 40 km away with a clear line of sight. However, the data extracted during this test may not have been reliable; therefore, our guess to the range of the device may be inaccurate. All of the data is able to be stored on a micro SD card. However, problems arose with opening multiple files; therefore, all the data must be stored on a single file. This is due to issues regarding data types in the code.
Meaning to Larger Project: This detector and the directional and ranging data it provides will permit better triggering and data collection for portions of the TARA experiment as well as collect data on the lightning strikes themselves to better correlate the events with cosmic rays.
http://www.telescopearray.org/tara/
Future Research: The lightning detection device is nearly ready to be implemented. The device still needs further field testing. If a method for calculating the distance of a lightning strike is needed, additional devices may need to be constructed. Additionally, cubic fits were applied to the angular calculation algorithm based off of light simulated from a strobe machine. If the angular reading is deemed to be inaccurate, data from lightning strikes should be used to refit the cubic fits. If quicker and more precise measurements are needed, this project could be redesigned using a time-to-digital converter instead of the Arduino Uno currently being used. However, a new code would have to be implemented.
Acknowledgements: We appreciate the assistance and guidance of the following during this project:
● Steven Prochyra, Graduate Student, University of Kansas, Lawrence, KS
● Samantha Conrad, Undergraduate Student, University of Kansas, Lawrence, KS
Quarked! Particle Physics Games
Name: Robert R. Nickel, Blue Valley North High School, Leawood, KS
Research Teacher Mentor: James Deane, Ottawa High School, Ottawa, KS
Research Mentors: Prof. Alice Bean, University of Kansas, Lawrence, KS
Purpose: The goal of the Quarked project is to make educational particle physics videos, games, and activities predominantly for pre-college students. Quarked provides a series of activites designed to generate interest in science among elementary and secondary students. Quarked is an important part of particle physics outreach at The University of Kansas because it simplifies the world of quantum physics in a way that aspiring scientists of all ages can understand. Quarked introduces particle physics concepts to students in a fun and engaging way.
Methods: The project uses ActionScript for programming, Adobe Photoshop for object creation, and Adobe Animate for animation of two-dimensional objects. Once the base code was created, I tested and revised the code in order to create the desired gameplay.
Results: I converted the Mass Matters game into a mobile Android app. Mass Matters involves shooting quarks and leptons and viewing their interaction within the higgs field to determine their mass. Converting the game to an app involved rewriting code for the Android platform, creating new graphics and animations, and extensive function and play testing on various computers, tablets, and smartphones. Additionally, I worked to improve the Quarked website by making the Quarked Club more functional and interesting. Previously, there was no direct incentive to encourage students to join the club. With these revisions, students need to correctly answer 10 particle physics questions. Being a part of the club allows students a sneak preview for upcoming games and one exclusive members-only game.
Meaning to Larger Project: The larger project is the collection of games and activities at www.quarked.org . My work expanded an important concept about the Higgs Boson to mobile users and reformed the Quarked Club to potentially be more popular. The Quarked website is intended to be a site that reaches students at early ages and helps them to understand some basic ideas of particle physics while showing the that thinking about science can be both fun and rewarding.
Future Research: The next step in the project will be to add more levels to Mass Matters to make the game more enjoyable and replayable. Once the app reaches both Android and iOS devices, it will be accessible to greater numbers of people.
Acknowledgements:
I appreciate the assistance and guidance of the following students during this project.
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Austin Irvine, Undergraduate Student, University of Kansas, Lawrence, KS
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Zach Harris, Research Assistant, University of Kansas, Lawrence, KS
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Hannah Gibson, Undergraduate Student, University of Kansas, Lawrence, KS
Background Data in Nuclear Interactions
Names: Sandhya Ravikumar, Lawrence Free State High School, Lawrence, Kansas
Research Teacher Mentor: James Deane, Ottawa High School, Ottawa, KS
Research Mentor: Prof. Philip Baringer, University of Kansas, Lawrence, KS
Purpose: This research is being conducted in an effort to reduce background data from the data collected from the CMS experiment at the LHC. Whenever experiments are conducted at the LHC, there is always a certain amount of redundant data that detracts from the useful data collected. I am hoping to eventually create a general fit function to eliminate the unnecessary data that comes with nuclear interaction experiments in any plot. Fit functions are essentially exponential functions created to match experimental data and adjust hardware measurements. The fit function serves the purpose of reducing accidental data collected by the sensitive instruments of the CMS pixel shield. It also adjusts the positioning of the machinery itself, as the machines shift from heating and cooling.
Methods: I began by familiarizing myself with the ROOT data analysis software. Anna Kropivnitskaya, a contact at CERN, provided me with Monte Carlo plots and plots from the CMS experiments I was also given a rough fit function program to refine to the graph. After fitting one graph, I moved on to the next, continuing with several graphs. I ran into several technical issues, mainly with software bugs and compatibility issues. ROOT operates best using a Linux or Mac OS, and having a Windows computer, I had to create a bootable USB drive using Ubuntu, a Linux distributor. Ubuntu had issues starting up with my computer, after which I had further issues getting it to work with ROOT. However, all issues were rectified relatively quickly. I had to use an older version of ROOT and use a different method of turning the USB drive into a bootable drive.
Results: I have created fit functions for various graphs, effectively eliminating background data and leaving a cleaner and more functional data set. By changing the fit program’s parameters, values, and operations, I have created several plots that are far more usable than they were in their original state. I achieved the results I hoped for, but I would like to continue working to create a more generalized fit function that would reduce background in any plot. I believe with more time and practice, the “universal” function should come rather easily.
Meaning to Larger Project: This research will help get to the truly useful and necessary data collected by nuclear interaction experiments. Once preliminary data is collected at the LHC, the unneeded and superfluous data can be eliminated by using various fit functions. The remaining data can be utilised easily and properly, without the obstruction of background. If a general fit function is created, the data and fit programs will be even more useful and applicable. The function also can be used to adjust the positioning of the equipment of the CMS tracker itself. As the machine heats and cools with use, it expands and contracts, causing components to shift. A version of the function can be used to measure and readjust the physical positioning of the trackers pixel shield and support beams.
Future Research: I have had success in creating individual fit functions for various plots by adjusting the parameters and values of the function. The logical next step is to create a universal fit function that would eliminate background from any CMS plot. By continuing to create fits for individual graphs, it would be relatively simple to establish a pattern and create a function that would only need to be adjusted slightly for differing graphs.
Acknowledgements:
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Eilish Gibson: Undergraduate Student, University of Kansas, Lawrence, KS
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Emily Smith: Undergraduate Student, University of Kansas, Lawrence, KS
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Anna Kropivnitskaya: Research Associate, University of Kansas, CERN, Geneva, Switzerland
T Quark Analysis from Generated Data
Names: Cole Brabec, Olathe Northwest High School
Research Teacher Mentor: James Deane, Ottawa High School, Ottawa, KS
Research Mentor: Prof. Philip Baringer, University of Kansas, Lawrence, KS
Purpose: The Purpose of this research is to investigate the possible existence of a fourth generation of quarks, specifically the T quark. This quark has many applications in modern physics such as solving the Hierarchy Problem or explaining the low Higgs Mass.
Note: The T quark is the particle formerly known as the t’ quark.
Methods: We used C++ and the software framework ROOT to analyze Monte Carlo files generated from MadGraph. We used these files to investigate the characteristics exhibited by the particles such as their phi, eta and transverse momentum. In order to determine what cut would maximize the data included from the signal file while minimizing the data included from the background file, we created a macro to calculate the figure of merit using the function FoM = S/Bk, where S is the amount of points within in the cuts from the signal file, B is the amount of points within the cuts from the background file and k is a scaling factor. The scaling factor was calculated using the relative sizes and probabilities of decay between the background and signal file; for these files it had a value of 802. The optimal cut would be used to determine which data received from the CMS exhibited signs of T quark decay
We also had to analyze the properties of the forward jet; the light quarks generated external to the T quark decay chain. This was difficult at first as in ROOT it is not possible to check for the grandparent or great-grandparent of a particle. To solve this issue, we looked at light quarks whose parents were other light quarks; this occurred only in the forward jet.
We had issues attempting to create cuts for both the Z boson and the forward jet, as these were not present in the background file. To work around this issue, we treated every light quark in the background file as the “forward jet”. For the Z boson, we were unable to develop a method to accurately imitate a presence of Z bosons in the background file and thus we were not able to generate meaningful cuts for them.
Results: Analyzing our cuts, it appears that the optimal cuts arePT > 410 GeVand < 2.4 for the top;HT > 1100; and PT < 570 and < 2.4for the Forward Jet at T quark mass 1 TeV. Cuts for other T quark masses were also generated and are available on a spreadsheet. We were also able to develop a piece of software to quickly and efficiently calculate the optimum cuts for different background and signal files.
Meaning to Larger Project: These cuts help refine the search range for finding the T quark. It will help us when analyzing real data to more quickly find the signs of a T quark. This data will also be used to help publish a paper about the T quark.
Future Research: The next step is analyze data directly from the CMS within our given cuts to see if it lines up with our predictions for the T quark. We also need a background file with Z bosons to better refine our cuts.
Acknowledgements:
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Zachary Flowers: Undergraduate Student, University of Kansas, Lawrence, KS
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Emily Smith: Undergraduate Student, University of Kansas, Lawrence, KS
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Dr. Alice Bean: Professor, University of Kansas, Lawrence, KS
Searching for Evidence of a 4th Generation Quark
Names: Grant Gollier, Bishop Seabury Academy, Lawrence, KS
Research Teacher Mentor: James Deane, Ottawa High School, Ottawa, KS
Research Mentor: Prof. Philip Baringer, University of Kansas, Lawrence, KS
Purpose: We are looking for evidence of a fourth generation quark which could help answer the hierarchy problem and specifically the odd discontinuity of mass.
Methods: I started by learning CERN’s ROOT data analysis framework. I used an online tutorial from Nevis Laboratories at Columbia University and help from fellow student researchers. I began by using demo files from the Nevis tutorial then proceeded to using ‘real’ files, plotting simple variables. In order to solve many of the problems I faced, I turned to both the ROOT documentation and the ROOT Talk forum. In addition to the learning curve of ROOT, I was new to C++ as well and had to learn the basic syntax and style of C++ as I went. After this introductory phase I began to look at two different decay modes for T (WbT and ZtT), plotting R, , Ht, and ptin one and two dimensional histograms. I then looked at these plots and decided upon cuts to maximize SB*k where S is the number of signal events, B is the number of background events, and k is the scale factor. This scale factor was necessary because I was only looking at one or two decay modes for as opposed to all possible decays. This scale factor accounts for the different probabilities/branching ratios.
Results: I developed multiple different scripts for processing these cuts. I looked at multiple T masses ranging from 800 GeV to 2.5 TeV. I then processed all the mass files with these cuts and passed the remaining events to plot , Ht, and pt.
Meaning to Larger Project: The hypothetical T quark offers a solution to the Hierarchy problem, which the solution to and discovery of this T would be pushing the boundaries of what is currently known in particle physics. Specifically, the cuts I was looking at would improve the quality of data I am gathering.
Future Research: As I ran short on time towards the end, I would like to spend more time analyzing the cuts I made and look for other ways to improve them. Also, following the use of these cuts more analysis would be needed to then identify the T and prove its existence.
Acknowledgements:
Without the help of many of the following people this project would not have been possible
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Zach Flowers, Student, University of Kansas
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Emily Smith, Student, University of Kansas
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Prof. Alice Bean, University of Kansas
[Link #1: http://www.nevis.columbia.edu/~seligman/root-class/
University of Kansas Summer 2016
Report is in the attached pdf.
Belle Electron-Positron Annihilation Analysis: A Search for a Dark Photon
Belle Electron-Positron Annihilation Analysis: A Search for a Dark Photon
Name: Margaret Lockwood, Lawrence High School
Research Teacher Mentor: James Deane, Ottawa High School, Ottawa, KS
Research Mentor: Prof. Dave Besson, University of Kansas, Lawrence, KS
Purpose: Analyzing positron-electron annihilations that result in either a positron-electron pair or two positron-electron pairs could provide support the theorized dark photon or other dark sector particles giving evidence for physics beyond the current standard model.
Methods: I first applied for and eventually received an account to access the Belle ( http://belle.kek.jp/ ) KEKB server. The data from the Belle asymmetric B factory collider in Japan provided me with data I could run scripts on to generate histograms of the invariant mass of collisions of interest. Any narrow spikes in the invariant mass histograms could indicate interesting physics, and potentially a dark photon. I installed a virtualbox to run Linux on my computer in order to become familiar with Linux commands. Waiting for my application approval, I started to become familiar with ROOT by following tutorials found on the internet and provided by other students. I learned more about the Belle collider in order to understand how and why the data I will be analyzing is produced. Once I gained access to the Belle server I ran a job using code a graduate student, Steven Prochyra, had created to start analyzing data. I used the generated data and information from Belle to become more familiar with the Belle framework. I started making histograms of the invariant mass from the data generated. I am starting to modify the macro that I used to analyze the data so that I can analyze different aspects of the data.
Results: I started editing the macro Steven Prochyra made to look at positron-positron and electron-electron collisions in order to use this data as background noise to compare to the electron-positron collisions. I made some invariant mass histograms electron-positron collisions, but it is difficult to know if I did these correctly or if the plots indicate anything interesting until I create more plots.
Meaning to Larger Project: Analyzing data from Asymmetric B Factories has led to evidence of CP (charge-parity) violations, information about rare decays, and can potentially provide support for new particles that may be a part of the dark sector. Finding a dark photon could lead to information about dark matter, the earliest moments of the Universe, new forces and other new particles outside of the standard model.
Future Research: I am going to continue to work on this project because I have only been working on getting over the Belle framework learning curve. The Belle data is a valuable resource that can be used for a vast amount of research projects regarding different decays. I will start creating my own macros to analyze different aspects of the data and continue to look for new physics including hints of the hidden sector.
Acknowledgement:
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Steven Prochyra, Graduate Student, University of Kansas
Investigation Into the Applicability of Solar Panels in Powering HiCal2
Investigation Into the Applicability of Solar Panels in Powering HiCal2
Names:
Finn Dobbs, Lawrence Free State High School, Lawrence, KS
Roxanna Hamidpour, Blue Valley North High School
Sabrea Platz, Lawrence Free State High School, Lawrence, KS
Asher Supernaw, Lawrence Free State High School, Lawrence, KS
Research Teacher Mentor:
James Deane, Ottawa High School, Ottawa, KS
Research Mentor:
Prof. Dave Besson, University of Kansas, Lawrence, KS
Purpose: Our purpose is to investigate the use of solar power for the HiCal2 balloon payload. The original battery system design limited the HiCal2 to 24 total hours of use in a 240 hour flight. Testing of solar panels in real world conditions is required to determine if the solar panels are sturdy enough to withstand the conditions at normal altitude in the antarctic atmosphere.
Methods: We tested the antenna efficacy by determining if a signal could be seen from thirty kilometers away. Successful signal transmission and reception at a distance of 30km is required because HiCal2 will fly from 25km-30km above the ground level in Antarctica on its flight. Antenna testing was accomplished by transmitting a signal and receiving on an ARIANNA antenna, then measuring this signal’s strength at 30 dBm above surrounding noise.
Once this data was collected, we began construction on an antenna to be flown on a weather balloon. Through testing multiple antenna designs with SWR measurements and wind resistance exercises for optimization of geometry, the Chicken Wire Antenna (CWA) was determined to be satisfactory for our experiment. With a proper transmission implement in place, a data collection strategy was devised. The CWA would transmit a signal, which would then be received by the ARIANNA antennas. An oscilloscope connected to the ARIANNA antenna record a waveform to floppy disk.
Aside from the CWA, the payload consisted of a data logger, GPS, amplifier, solar panel, and a voltage controlled oscillator (VCO). The data logger was monitored by the solar panel and served to ensure that the solar panel continuously supplied power to the payload. When devising a plan to transmit the signal, an amp circuit system was investigated, but the transmitted signal was variable and unpredictable. Instead of this amp circuit system, we used the VCO as the means of producing a signal that would then be transmitted by the CWA. The VCO’s tuning input voltage was directly connected to the solar panel, meaning that the frequency of the signal transmitted by the CWA correlated directly to the voltage supplied by the solar panel. This payload was then constructed and secured to the balloon.
Results: The weather balloon and payload were launched successfully, but we could not successfully retrieve ground station and logged data. The ground station based oscilloscope saved the same waveform multiple times rather than the expected real-time data. Without long-term data from the received VCO signal, we cannot determine the stability of the solar panel system voltage over time. After the flight, we were unable to locate the payload, and as of the writing of this abstract it remains lost. If we do retrieve the payload, we could analyze data from the data logger to determine the performance of the solar panel system voltage over time.
Meaning to Larger Project: The purpose of our summer research was to devise an alternate power source for the HiCal2 experiment that was lighter and more reliable than batteries. We wanted to test solar panels in a real world environment with both temperature inversion and potential weather conditions. We were not able to answer these questions conclusively with this launch, but future balloon launches will build on these successes and failures.
Future Research: A second balloon launch is planned for the near future, which will include a more reliable retrieval process. A reliable retrieval is vital in developing confidence in future balloon launches so that costly equipment can be used without fear of significant losses.
Acknowledgements:
We appreciate the assistance and guidance of the following students during this project.
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Conner Brown: Undergraduate Student, University of Kansas
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Joshua Macy: Senior Lead Undergraduate Student, University of Kansas
Lightning Detection and Triggering for the TARA Experiment
Names: Bennett Haase-Divine, Lawrence Freestate High School
Pierce Giffin, Shawnee Mission East High School
Research Teacher Mentor: James Deane, Ottawa High School, Ottawa, KS
Research Mentor: Prof. Dave Besson, University of Kansas, Lawrence, KS
Purpose: The purpose of our project was to accurately detect flashes of lightning as well as determining their approximate position and time of strike so that other devices involved in the TARA project can study and collect data from flashes of lightning while they’re still striking.
Methods: For light detection, we used several photoresistors and an arduino board that read the voltage off of each resistor. If the voltage was high enough, the program would identify it as a lightning strike. As soon as a flash of lightning is detected, a signal is sent out to alert other devices that lightning has struck. To calculate the angle the strike occurred relative to the device, we see how high the voltages are on each photoresistor relative to one another and weight each voltage with the photoresistor’s assigned angle. After a flash of lightning is detected, a microphone starts listening to the environment for the thunder. Once it picks up a loud sound, it calculates how far away the strike of lightning occurred. After all the data is collected, it is stored on a micro SD card inside of the device.
Results: Almost all of the necessary operations work properly with a simulated strobe machine. The device is capable of detecting nearly 100% of simulated flashes and calculating the correct angle within about 10%. The signal is capable of being sent out to other devices within 5 milliseconds. The device can accurately identify two flashes of lightning within 20 milliseconds of each other. Since a single lightning strike flashes once then flashes again about 30 milliseconds later (and can repeat several more times), the device is capable of detecting a strike of lightning on the first flash then sending out a signal to other devices to collect data on other flashes. The sound device works accurately. We are able to calculate the distance within 10 meters. Without simulating with actual lightning, it is unsure as to how far away a lightning strike could occur without being detected by the device. All of the data is able to be stored on a micro SD card. However, problems arose with opening multiple files; therefore, all the data must be stored on a single file.
Meaning to Larger Project: This detector and the directional and ranging data it provides will permit better triggering and data collection for portions of the TARA experiment. http://www.telescopearray.org/tara/
Future Research: The lightning detection device is nearly ready to be implemented. The device still needs to be field tested and, if possible, store the data on multiple files. If quicker and more precise measurements are needed, this project could be redesigned using a time-to-digital converter instead of the Arduino Uno currently being used. However, a new code would have to be implemented.
Acknowledgements:
We appreciate the assistance and guidance of the following students during this project.
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Steven Prochyra, University of Kansas
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Samantha Conrad, University of Kansas