Project GRAND

Last updated
Project GRAND ("Gamma Ray Astrophysics at Notre Dame")
ND GRAND 02.jpg
Project GRAND, 2004
Location(s) University of Notre Dame, Notre Dame, IN
Coordinates41°42′41″N, 86°14′20″W 41°42′41″N86°14′20″W / 41.71139°N 86.23889°W / 41.71139; -86.23889
OrganizationNotre Dame Department of Physics and Astronomy, National Science Foundation
Altitude220 m
Built1987-1996
Diameter64, 1.29 m2 proportional wire chambers
Angular resolution 0.25°
Collecting area83 m2
Website https://www3.nd.edu/~grand/
World location map (equirectangular 180).svg
Red pog.svg
Location of Project GRAND ("Gamma Ray Astrophysics at Notre Dame")
[ edit on Wikidata]

Project GRAND is a cosmic ray observatory located on the University of Notre Dame campus. [1] [2] The observatory features a grid of sixty-four proportional wire chamber (PWC) particle detectors positioned within a 10,000 m2 field. Project GRAND was designed and built by Notre Dame professor emeritus John Poirier and his students. [2] [3] The observatory operated mainly between 1989 and 2011. [4] Project GRAND detected cosmic rays from the sun and extrasolar sources. [5] [6] Project GRAND was also able to discern the effect of atmospheric temperature and pressure on cosmic ray surface counts. [7]

Contents

Concept and features

Cosmic rays were discovered in 1912 by Austrian physicist Victor F. Hess for which he won the 1936 Nobel Prize in physics. [8] Cosmic rays are particles, mostly protons, that are emitted by the sun and extrasolar sources. These particles impact earth's atmosphere to produce showers of particles ("extensive air showers" or EAS) that can be detected from the surface. In 1983, German physicists Wilhelm Stamm and Manfred Samorski were able to link cosmic rays to a source in space named Cygnus X-3 (the third brightest x-ray emitting object in the constellation Cygnus). [9] [2] Cygnus X-3 emits two major types of particles: protons and gamma ray photons. The gamma rays fall within two categories, "very high energy" (1012 eV) and "ultra high energy" (1015 eV). Of these categories, ultra high energy gamma rays can be observed using ground based cosmic ray detectors. [9] [10]

View from the north of Project GRAND, 2004, Calvin Swartzendruber. ND GRAND 01.jpg
View from the north of Project GRAND, 2004, Calvin Swartzendruber.

Professor emeritus John Poirier of the University of Notre Dame founded Project GRAND in the late 1980s. Poirier obtained his Ph.D. in particle physics from Stanford University, and he later performed research at the Serpukhov accelerator in Russia and at Fermilab near Chicago. [11] [2] Poirier joined the Notre Dame Department of Physics faculty in 1964. [12] Poirier later pursued the study of cosmic rays and their sources in space. [3] He initially made plans to build a conventional optical detector that would be placed in a northern Indiana soybean field, [13] [14] [15] but a leading expert in scintillation detector technology from Krakow, Poland [14] then visiting the Notre Dame campus convinced Poirier to pursue a different approach, one that wouldn't be dependent upon weather conditions. [2] Poirier employed Monte Carlo simulations to design a scintillator-based cosmic ray observatory that would detect extensive air showers produced by ultra high energy gamma rays and protons. [16] The observatory, named Project GRAND, would be able to pinpoint the sources of cosmic ray particles to an angular resolution of 0.25° (an apparent angle of half the size of a full moon). Poirier presented this plan in a 1987 paper for the 20th International Cosmic Ray Conference held in Moscow. [17] [18] GRAND is an acronym for "Gamma Ray Astrophysics at Notre Dame". [2] The observatory would be built with the assistance of the National Science Foundation (NSF) as well as funds from the University of Notre Dame and private individuals. [7] [2] [19] Newspaper articles about Poirier and Project GRAND were published in the January 9, 1989 and November 19, 1989 editions of the South Bend Tribune. [14] [2]

Project GRAND schematic. Project GRAND Map.jpg
Project GRAND schematic.
Project GRAND wooden "hut" schematic. Each hut features 4 proportional wire chambers (each containing two sets of tungsten wires) to detect cosmic rays. Hut Figure Looking North.jpg
Project GRAND wooden "hut" schematic. Each hut features 4 proportional wire chambers (each containing two sets of tungsten wires) to detect cosmic rays.

In its heyday, Project GRAND utilized a set of 64 cosmic ray detecting installations that were located on a level field north of the Notre Dame main campus. Each of the 64 installations employed a set of eight vertically stacked proportional wire chambers (PWCs). [20] [21] (George Charpak won a 1992 Nobel Prize in physics for inventing the PWC.) [22] At Project GRAND, each PWC chamber features 160 orthogonally positioned tungsten wires (two sets of 80 wires) sealed within an atmosphere consisting of argon and carbon dioxide (80% and 20% respectively). Cosmic ray "hits" were registered by the detection of ionized gases as voltage differences in the tungsten wires. [23] [24] The 64 installations, termed "huts", are plywood buildings arrayed in an 8 by 8 grid covering an area of 10,000 m2 (a 100 m by 100 m field). The grid is oriented directly north to south and, along with the stacked PWCs, allowed estimation of the angles of entry of cosmic ray induced particles. [25]

Extensive air showers display a cone of particles that impact earth's surface in an approximate 200 m diameter circular area. [9] At Project GRAND, near simultaneous detections within multiple huts established the occurrences of an extensive air showers. [26] [20] A steel plate positioned above the bottom PWC in each hut was used to detect muons. Muons are heavy, [27] short-lived cousins of the electron that are generated in earth's atmosphere by the impact of cosmic rays. [28] The steel plate also allowed discrimination between air showers generated by gamma ray photons and those generated by protons, and the detection of muons enabled the differentiation of these sources of air showers. [20] According to Poirier, in his proposal for the experiment, background protons would be reduced to zero by the detection of muons, and the detection of muons could then be linked to extended air showers produced by ultrahigh energy gamma rays. [17]

Each of the 64 huts was connected to a central trailer where data from the experiment was accumulated. [17] The data trailer had been obtained from NASA surplus and may have been used as a quarantine facility for Mercury and Gemini mission astronauts. [24] [29]

Discoveries, educational opportunities

The Project GRAND experiment operated between 1989 and 2011. [4] As stated, the observatory received funds from the National Science Foundation. After construction, the main expense of the experiment was the purchase of the argon gas used in the PWCs. [24]

Interior view of a Project GRAND hut. 4 proportional wire chambers are featured (each containing two sets of tungsten wires). The red component supports a 5 cm thick steel plate used to distinguish muons from electrons. Project GRAND Proportional Wire Chambers 2024.jpg
Interior view of a Project GRAND hut. 4 proportional wire chambers are featured (each containing two sets of tungsten wires). The red component supports a 5 cm thick steel plate used to distinguish muons from electrons.

At the 28th International Cosmic Ray Conference held in Tsubuka, Japan [30] in 2003, Professor Poirier presented results suggesting that Project GRAND may have been able to detect excess muons from cosmic ray bursts visible from the observatory. Poirier used data from the BATSE experiment that was part of the NASA's Compton Gamma Ray Observatory. [6] [31] In particular, he demonstrated that a 2.7σ statistical significance was obtained for the detection of muons at Project GRAND from gamma ray burst GRB 971110. [6]

Results of Project GRAND observations of two solar flares were reported at the 30th International Cosmic Ray Conference held in Mérida, Mexico [32] in 2007. [33] On April 15, 2001, an X14 solar flare erupted on the sun and Project GRAND was able to detect excess muons from this event at a statistical level of 6.1σ. [5] Project GRAND also detected excess muons with a confidence of 9.9σ from an X7.1 solar flare that occurred on January 20, 2005. [34] Another phenomenon related to solar flares, the Forbush decrease, was also observed using Project GRAND data. A Forbush decrease is a temporary lowering of the detectable flux of extrasolar cosmic rays due to the magnetic interference of a solar coronal mass ejection (CME). A decrease in extrasolar cosmic ray flux was detected at Project GRAND after the September 11, 2005 CME and reported at the Mérida conference. [25] [35]

An earlier Forbush decrease had been observed after the CME of October 28, 2003. According to Christopher D'Andrea's Ph.D thesis, the muon flux dropped by 8% after the October 29 CME and a change of direction in associated cosmic ray particles was observed. This change of direction may have been linked to the interaction of earth's magnetic field with that of the CME. [25]

Project GRAND NASA surplus data trailer, July 2024. Project GRAND Data Trailer 2024.jpg
Project GRAND NASA surplus data trailer, July 2024.

At the 32nd International Cosmic Ray Conference held in Beijing [36] in 2011, Professor Poirier was able to demonstrate a relationship between muon flux and atmospheric temperature and pressure using data from Project GRAND. The experiment had been detecting muons since 1995, and the entire array collected muons at a rate of approximately 2,000 per second. Poirier found that higher atmospheric pressures caused a decrease in muon detections. He also determined that higher temperatures likewise produce lower rates of muon detection in the experiment. [37] At this same conference, Poirier unveiled the results of a 117-day run of muon detections at the observatory in 2007. Muon fluxes throughout a 24-hour period differed and exhibited daily highs and lows. A longer-term variation over the entire observing period was also observed with a high flux of muons occurring in October 2008. Poirier attributed this seasonal flux to the location of earth within the solar system's magnetic field (interplanetary magnetic field, IMF). [7]

Graduate students as well as undergraduate and high school teachers and students have performed research and maintenance of the Project GRAND experiment. [33] [38] Using Project GRAND data under the aegis of Dr. Poirier, Younan Lu earned a Ph.D. in 1991 [39] and Christopher D'Andrea earned a Ph.D. in 2006. [25] In 2007 it was reported that six Notre Dame undergraduate students had performed research at Project GRAND and wrote three theses. [33] During summers, undergraduate students from other universities have participated in Project GRAND through Notre Dame's research experiences for undergraduates (REU) program. [40] [41] In 2004, Cornell REU student David Levitan updated the experiment's Fortran code to C. [25] Levitan went on to earn a Ph.D in astrophysics from Caltech and is now a data scientist for Microsoft. [42] Local high school teachers and students have also worked at Project GRAND through Notre Dame's research experiences for high school students (REHS) and research experiences for teachers (RET) programs [33] administered by the QuarkNet Center at the University of Notre Dame. [38] [43] According to QuarkNet National Staff Teacher Ken Cecire, [44] "the project serves as a valuable outreach tool for high school students and teachers to study astrophysics." [45]

See also

Related Research Articles

<span class="mw-page-title-main">Muon</span> Subatomic particle

A muon is an elementary particle similar to the electron, with an electric charge of −1 e and spin-1/2, but with a much greater mass. It is classified as a lepton. As with other leptons, the muon is not thought to be composed of any simpler particles.

<span class="mw-page-title-main">Cosmic ray</span> High-energy particle, mainly originating outside the Solar System

Cosmic rays or astroparticles are high-energy particles or clusters of particles that move through space at nearly the speed of light. They originate from the Sun, from outside of the Solar System in our own galaxy, and from distant galaxies. Upon impact with Earth's atmosphere, cosmic rays produce showers of secondary particles, some of which reach the surface, although the bulk are deflected off into space by the magnetosphere or the heliosphere.

The Greisen–Zatsepin–Kuzmin limit (GZK limit or GZK cutoff) is a theoretical upper limit on the energy of cosmic ray protons traveling from other galaxies through the intergalactic medium to our galaxy. The limit is 5×1019 eV (50 EeV), or about 8 joules (the energy of a proton travelling at ≈ 99.99999999999999999998% the speed of light). The limit is set by the slowing effect of interactions of the protons with the microwave background radiation over long distances (≈ 160 million light-years). The limit is at the same order of magnitude as the upper limit for energy at which cosmic rays have experimentally been detected, although indeed some detections appear to have exceeded the limit, as noted below. For example, one extreme-energy cosmic ray, the Oh-My-God Particle, which has been found to possess a record-breaking 3.12×1020 eV (50 joules) of energy (about the same as the kinetic energy of a 95 km/h baseball).

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<span class="mw-page-title-main">Air shower (physics)</span> Cascade of atmospheric subatomic particles

Air showers are extensive cascades of subatomic particles and ionized nuclei, produced in the atmosphere when a primary cosmic ray enters the atmosphere. Particles of cosmic radiation can be protons, nuclei, electrons, photons, or (rarely) positrons. Upon entering the atmosphere, they interact with molecules and initiate a particle cascade that lasts for several generations, until the energy of the primary particle is fully converted. If the primary particle is a hadron, mostly light mesons like pions and kaons are produced in the first interactions, which then fuel a hadronic shower component that produces shower particles mostly through pion decay. Primary photons and electrons, on the other hand, produce mainly electromagnetic showers. Depending on the energy of the primary particle, the detectable size of the shower can reach several kilometers in diameter.

The Chicago Air Shower Array (CASA) was a significant ultra high high-energy astrophysics experiment operating in the 1990s. It consisted of a very large array of scintillation detectors located at Dugway Proving Grounds in Utah, USA, approximately 80 kilometers southwest of Salt Lake City. The full CASA detector, consisting of 1089 detectors began operating in 1992 in conjunction with a second instrument, the Michigan Muon Array (MIA), under the name CASA-MIA. MIA was made of 2500 square meters of buried muon detectors. At the time of its operation, CASA-MIA was the most sensitive experiment built to date in the study of gamma ray and cosmic ray interactions at energies above 100 TeV (1014 electronvolts). Research topics on data from this experiment covered a wide variety of physics issues, including the search for gamma rays from Galactic sources (especially the Crab Nebula and the X-ray binaries Cygnus X-3 and Hercules X-1) and extragalactic sources (active Galactic nuclei and gamma-ray bursts), the study of diffuse gamma-ray emission (an isotropic component or from the Galactic plane), and measurements of the cosmic ray composition in the region from 100 to 100,000 TeV. For the topic of composition, CASA-MIA worked in conjunction with several other experiments at the same site: the Broad Laterial Non-imaging Cherenkov Array (BLANCA), the Dual Imaging Cherenkov Experiment (DICE) and the Fly's Eye HiRes prototype experiment. CASA-MIA operated continuously between 1992 and 1999. In summer 1999, it was decommissioned.

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<span class="mw-page-title-main">Neutrino detector</span> Physics apparatus which is designed to study neutrinos

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References

  1. ↑ "The University of Notre Dame (Project GRAND)". www3.nd.edu. Retrieved 2024-06-25.
  2. 1 2 3 4 5 6 7 8 Rumbach, Dave (Nov 19, 1989). "Cosmic Ray Mystery". South Bend Tribune. p. 12. Retrieved Jun 25, 2024.
  3. 1 2 Wiegard, Sandra (Nov 29, 1989). "ND receives equipment for study of cosmic rays of star Cygnus X-3" (PDF). The Observer. p. 3. Retrieved Jul 24, 2024.
  4. 1 2 "Publications". www3.nd.edu. Retrieved 2024-06-25.
  5. 1 2 Poirier, J.; D'Andrea, C. (Nov 2002). "Ground level muons in coincidence with the solar flare of April 15, 2001". Journal of Geophysical Research: Space Physics. 107 (A11). arXiv: astro-ph/0211490 . doi:10.1029/2001JA009187. ISSN   0148-0227.
  6. 1 2 3 Poirier, J.; D'Andrea, C.; Gress, J.; Race, D. (2003). "Search for sub-TeV gamma rays in coincidence with gamma ray bursts". Physical Review D. 1 (4): 1–4. arXiv: astro-ph/0306370 . doi:10.1103/PhysRevD.67.042001.
  7. 1 2 3 Poirier, J.; Catanach, T. (2011). "Periodic Variations in Muon Flux at Project GRAND" (PDF). 32nd International Cosmic Ray Conference, Beijing 2011. II: 173–176.
  8. ↑ "Victor F. Hess, Physicist, Dies; Shared the Nobel Prize in 1936; Was Early Experimenter on Conductivity of Air—Taught at Fordham Till 1958". The New York Times. 1964-12-19. ISSN   0362-4331 . Retrieved 2024-07-10.
  9. 1 2 3 MacKeown, P. K.; Weekes, T. C. (1985-11-01). "Cosmic rays from Cygnus X-3". Scientific American. 253 (5): 60–69. Bibcode:1985SciAm.253e..60M. doi:10.1038/scientificamerican1185-60. ISSN   0036-8733.
  10. ↑ "Mysterious Particles May Upset Theories on Radiation From Space". The New York Times. ISSN   0362-4331 . Retrieved 2024-06-25.
  11. ↑ Dame, Marketing Communications: Web | University of Notre. "John Poirier". Department of Physics and Astronomy. Retrieved 2024-06-26.
  12. ↑ "Dr. John Poirier to Notre Dame". Times Clarion (Harlowton, Montana). Jun 18, 1964. p. 1. Retrieved Jul 12, 2024.
  13. ↑ Rumbach, Dave (Jan 22, 1986). "Commission delays star-study rezoning". South Bend Tribune. p. 23. Retrieved Jul 12, 2024.
  14. 1 2 3 Benchik, Marilyn (Jan 9, 1989). "New challenge to be tackled on N.D. turf". South Bend Tribune. p. 10. Retrieved Jul 12, 2024.
  15. ↑ Rumbach, Dave (Feb 19, 1986). "Plan panel clears clubhouse, offices, science experiment". South Bend Tribune. pp. B3. Retrieved Jul 24, 2024.
  16. ↑ Poirier, J.; Linsley, J.; Mikocki, S. (1987-09-01). "Angular distributions of secondary charged particles in showers initiated by gammas and protons". Physical Review D. 36 (5): 1378–1380. doi:10.1103/PhysRevD.36.1378.
  17. 1 2 3 Poirier, J.; Funk, E.; Losecco, J.; Mikocki, S.; Rettig, T. (1987). "1987ICRC....2..438P Page B438". International Cosmic Ray Conference. 2: 438. Bibcode:1987ICRC....2..438P . Retrieved 2024-06-25.
  18. ↑ "CERN Document Server: 20th International Cosmic-ray Conference". CERN Document Server.
  19. ↑ "Faculty grants announced" (PDF). The Observer. Sep 22, 1988. p. 6. Retrieved Jul 24, 2024.
  20. 1 2 3 Poirier, J.; Canough, G.; Gress, J.; Mikocki, S.; Rettig, T. (1990). "The Project GRAND extensive air shower array". Nuclear Physics B. 14A: 143–146. doi:10.1016/0920-5632(90)90410-V.
  21. ↑ Gress, J.; Mikocki, S.; Poirier, J.; Rettig, T. (1990). "1990ICRC...10..335G Page J335". 21st International Cosmic Ray Conference (Icrc21). 10: 335. Bibcode:1990ICRC...10..335G . Retrieved 2024-07-10.
  22. ↑ "The Detector Modules". www3.nd.edu. Retrieved 2024-07-08.
  23. ↑ Gress, J.; Mikocki, S.; Poirier, J.; Rettig, T. (1990). "1990ICRC...10..335G Page J335". 21st International Cosmic Ray Conference (Icrc21). 10. Bibcode:1990ICRC...10..335G . Retrieved 2024-07-12.
  24. 1 2 3 "Project GRAND In-depth Description". www3.nd.edu. Retrieved 2024-07-03.
  25. 1 2 3 4 5 D'Andrea, Christopher (Dec 2006). "Analysis of Ground Level Muons, Solar Flares, and Forbush Decreases: A Dissertation". Graduate Program in Physics, Notre Dame, Indiana.
  26. ↑ Gress, J. (1997). "1997ICRC....6..221G Page F221". International Cosmic Ray Conference. 6: 221. Bibcode:1997ICRC....6..221G . Retrieved 2024-07-10.
  27. ↑ "Scientist tells discovery of fat electrons". Binghamton Press and Sun-Bulletin. May 2, 1938. p. 10. Retrieved Jul 24, 2024.
  28. ↑ "DOE Explains...Muons". Energy.gov. Retrieved 2024-07-24.
  29. ↑ "ND QuarkNet Center - Trailer". sites.google.com. Retrieved 2024-07-10.
  30. ↑ "28th International Cosmic Ray Conference, Tsukuba, Japan, 2003". CERN Document Server.
  31. ↑ "BATSE". NASA Gamma Ray Astrophysics NSSTC. Retrieved Jul 9, 2024.
  32. ↑ "30th International Cosmic Ray Conference, Merida, Mexico, 2007". CERN Document Server.
  33. 1 2 3 4 Poirier, J.; D'Andrea, C.; Fidler, E.; Gress, J.; Herrera, M.; Hemphill, P.; Schwartzendruber, C. (2007). "Status report on project GRAND" (PDF). 30th International Cosmic Ray Conference, Merida, Mexico, 2007.
  34. ↑ D'Andrea, C.; Poirier, J. (2005-07-28). "Ground level muons coincident with the 20 January 2005 solar flare". Geophysical Research Letters. 32 (14). doi:10.1029/2005GL023336. ISSN   0094-8276.
  35. ↑ Poirier, J.; Herrera, M.; Hemphill, P.; D'Andrea, C. (2008-07-14), A study of the Forbush decrease event of September 11, 2005 with GRAND, arXiv: 0807.2256
  36. ↑ "32nd International Cosmic-ray Conference, Beijing, 2011". CERN Document Server.
  37. ↑ Poirier, J.; Catanach, T. (2011). "Atmospheric Effects on Muon Flux at Project GRAND" (PDF). 32nd International Cosmic Ray Conference, Beijing 2011. II: 349–351.
  38. 1 2 "Notre Dame QuarkNet Center 2014 Annual Report". QuarkNet. 2014-09-24. Retrieved 2024-07-09.
  39. ↑ Lu, Younan (Oct 1991). "Studies of Cosmic Rays Using Proportional Wire Chambers: A Dissertation". Department of Physics, University of Notre Dame.
  40. ↑ Ball, Molly. "Correction Methods for Project GRAND Data". physics.nd.edu. Retrieved Jul 10, 2024.
  41. ↑ Ball, Molly. "Molly Ball, The Ohio State University". ResearchGate. Retrieved Jul 10, 2024.
  42. ↑ "David Levitan's Homepage". www.dlevitan.com. Retrieved 2024-07-11.
  43. ↑ "Project GRAND: People". ND QuarkNet Center. Retrieved Jul 10, 2024.
  44. ↑ Dame, Marketing Communications: Web | University of Notre. "Kenneth Cecire". Department of Physics and Astronomy. Retrieved 2024-07-22.
  45. ↑ "UND Project GRAND Group Abstract". QuarkNet. 2014-09-17. Retrieved 2024-07-22.
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