[{"data":1,"prerenderedAt":-1},["ShallowReactive",2],{"detail-sidebar-cat-0-en-105":3,"doc-seo-636550-105":59,"doc-detail-636550-en":130},{"code":4,"msg":5,"data":6},0,"success",[7,13,18,23,28,33,38,43,48,51,55],{"id":8,"doc_module":4,"doc_module_name":9,"category_name":10,"show_sort_weight":11,"slug":12},1,"Document","Story & Novel",90,"story-novel",{"id":14,"doc_module":4,"doc_module_name":9,"category_name":15,"show_sort_weight":16,"slug":17},2,"Literature",80,"literature",{"id":19,"doc_module":4,"doc_module_name":9,"category_name":20,"show_sort_weight":21,"slug":22},4,"Exam",70,"exam",{"id":24,"doc_module":4,"doc_module_name":9,"category_name":25,"show_sort_weight":26,"slug":27},5,"Comic",60,"comic",{"id":29,"doc_module":4,"doc_module_name":9,"category_name":30,"show_sort_weight":31,"slug":32},6,"Technology",50,"technology",{"id":34,"doc_module":4,"doc_module_name":9,"category_name":35,"show_sort_weight":36,"slug":37},7,"Healthcare",40,"healthcare",{"id":39,"doc_module":4,"doc_module_name":9,"category_name":40,"show_sort_weight":41,"slug":42},8,"Research & Report",30,"research-report",{"id":44,"doc_module":4,"doc_module_name":9,"category_name":45,"show_sort_weight":46,"slug":47},9,"Religion & Spirituality",20,"religion-spirituality",{"id":46,"doc_module":4,"doc_module_name":9,"category_name":49,"show_sort_weight":46,"slug":50},"World Cup","world-cup",{"id":52,"doc_module":4,"doc_module_name":9,"category_name":53,"show_sort_weight":52,"slug":54},10,"Lifestyle","lifestyle",{"id":56,"doc_module":4,"doc_module_name":9,"category_name":57,"show_sort_weight":24,"slug":58},19,"General","general",{"code":4,"msg":60,"data":61},"ok",{"site_id":62,"language":63,"slug":64,"title":65,"keywords":66,"description":67,"schema_data":68,"social_meta":123,"head_meta":125,"extra_data":127,"updated_unix":129},105,"en","cosmic-ray-studies-with-the-minos-detectors-ahabig-umd","Cosmic Ray Studies with the MINOS Detectors - A.Habig, UMD","","Cosmic ray studies using the MINOS detectors describe how a muon-neutrino beam and layered scintillator/steel calorimeters probe neutrino disappearance through neutrino oscillations. The poster details the Far Detector location and performance versus the Near Detector, focusing on cosmic-ray muons that penetrate rock overburden. It reports measurements of the cosmic-ray muon charge ratio above 1 TeV, links muon rates to atmospheric temperature via an effective isothermal temperature, and presents cosmic-ray shadow observations of the Sun and Moon.",{"@graph":69,"@context":122},[70,84,105],{"@type":71,"itemListElement":72},"BreadcrumbList",[73,77,79,82],{"item":74,"name":75,"@type":76,"position":8},"https://docshare.wps.com","Home","ListItem",{"item":78,"name":9,"@type":76,"position":14},"https://docshare.wps.com/document/",{"item":80,"name":40,"@type":76,"position":81},"https://docshare.wps.com/document/research-report/",3,{"item":83,"name":65,"@type":76,"position":19},"https://docshare.wps.com/document/cosmic-ray-studies-with-the-minos-detectors-ahabig-umd/636550/",{"url":83,"name":65,"@type":85,"image":86,"author":91,"headline":65,"publisher":94,"fileFormat":97,"inLanguage":63,"description":67,"dateModified":98,"datePublished":99,"encodingFormat":97,"isAccessibleForFree":100,"interactionStatistic":101},"DigitalDocument",{"url":87,"@type":88,"width":89,"height":90},"https://docshare.wps.com/thumbnails/cosmic-ray-studies-with-the-minos-detectors-ahabig-umd/636550.png","ImageObject",300,407,{"name":92,"@type":93},"Aran","Person",{"url":74,"name":95,"@type":96},"DocShare","Organization","application/pdf","2026-11-04","2026-10-22",true,{"@type":102,"interactionType":103,"userInteractionCount":39},"InteractionCounter",{"@type":104},"ViewAction",{"@type":106,"mainEntity":107},"FAQPage",[108,114,118],{"name":109,"@type":110,"acceptedAnswer":111},"What is the main physics goal of the MINOS experiment described here?","Question",{"text":112,"@type":113},"The MINOS experiment uses a muon-neutrino beam and two layered detector systems to search for muon-neutrino disappearance, enabling tests of neutrino oscillations.","Answer",{"name":115,"@type":110,"acceptedAnswer":116},"How is the cosmic-ray muon charge ratio measurement carried out?",{"text":117,"@type":113},"Muons are separated by charge using the MINOS magnetic field, using forward/reverse magnetic field configurations to cancel detector and field asymmetries and applying charge-selection cuts.",{"name":119,"@type":110,"acceptedAnswer":120},"How does atmospheric temperature affect the underground muon rate in this study?",{"text":121,"@type":113},"Higher atmospheric temperatures reduce air density, increasing decay fractions of secondary particles and leading to a higher deep underground muon rate. The analysis uses an effective isothermal temperature and finds a correlation between changes in muon rate and temperature.","https://schema.org",{"og:url":83,"og:type":124,"og:title":65,"og:site_name":95,"og:description":67},"article",{"robots":126,"canonical":83},"index,follow",{"doc_id":128,"site_id":62},636550,1793109147,{"code":4,"msg":5,"data":131},{"doc_id":128,"user_id":132,"nickname":92,"user_avatar":133,"doc_module":4,"category_id":39,"category_name":40,"doc_title":65,"doc_description":67,"doc_content":134,"file_id":135,"file_url":136,"file_type":137,"file_size":138,"view_count":39,"is_deleted":4,"is_public":8,"is_downloadable":8,"audit_status":8,"page_count":8,"language":139,"language_code":63,"site_id":62,"html_lang":63,"table_of_contents":140,"faqs":141,"seo_title":142,"seo_description":67,"update_tm":143,"read_time":81},137455076865,"https://ap-avatar.wpscdn.com/davatar_29158cc5080c5b710cf443261637dec0","Cosmic Ray Studies with the MINOS Detectors  \nA.Habig, UMD, for the MINOS Collaboration  \nThe MINOS Experiment  \nFar detector   \nNeutrino beam   \nThe MINOS experiment uses two layered scintillator and steel detectors along with a muon neutrino beam to search for ν μ disappearance, and thus neutrino oscillations.  \nThe Far Detector is situated in a former iron mine in the Soudan Underground Mine State Park in Northeastern MN, 700 m (2070 mwe) below the surface. This 5.4 kt steel/scintillator calorimeter measures the neutrino flux after they have traveled the 735 km baseline. It also detects atmospheric neutrinos at a rate of several per week, and is the first magnetized atmospheric neutrino detector, able to discriminate between ν μ and ν μ on an event-by-event basis. The similar 1 kt Near Detector is 100 m (220 mwe) underground at Fermilab.  \nThis poster discusses the science being done with the high energy cosmic ray muons which penetrate the rock overburden and are seen by the detectors. The typical surface energy of those seen at the Far Detector are ~1 TeV (coming from ~8 TeV primary cosmic rays) and ~110 GeV at the Near Detector (~900 GeV primaries) .  \nWatch MINOS Far Detector data arrive (mostly cosmic μ at ½ Hz) live on the web:  \n[http://farweb.minos-soudan.org/events/](http://farweb.minos-soudan.org/events/)  \nVeto shield, planes, and cosmic muon tracks  \nAdditional layers of scintillator on the top and sides of the detector provide a veto for entering cosmic ray muons which might otherwise slide down between layers and appear to be a contained vertex, increasing the efficiency of finding muon tracks which would otherwise slip through the vertical spaces between planes.  \nLeft: The detector seen from above showing a partially installed veto shield (the silver sheets) and the layered nature of the MINOS Far Detector (here with plane 483 of 485 installed) .  \nF R F  \nRight: a face-on view of a cosmic ray muon traversing the MINOS Far Detector, with a cluster of veto shield hits (circled) clearly showing the muon entrance point.  \nCharge Ratio of Cosmic Ray μ  \nGeometric mean of forward and reversed sets cancels out detector and Bfield asymmetries (seen here in ND data)  \nND: Use 37.8 days each Forward/Reverse Bfield  \n676k μ survive harsh track quality cuts, resulting in only a 0.21% charge mis-ID rate.  \nFD: Use 610 (F) and 202 (R) days data, 1.2 million μ remain after tight charge-selection cuts (only 3.2% of total μ sample)  \nFD: r = 1.374 ± 0.004 (stat.) 00 ..012010 (syst.)  \nPhys. Rev. D 76 052003. (2007)  \nParameterize muon yield from p and K mesons, fit to data  \n• best fit values: fπ+ = 0.55 fK+ = 0.67  \n•Implies production ratio of π +/π - ~1.2 and production ratio of K+/K- ~ 2.0, providing the first evidence for associated production at TeV energies.  \nND: r = 1.270 ± 0.003 (stat.) ± 0.013 (syst.)   \nGoal: measurement of the charge ratio of cosmic ray muons above 1 TeV surface energy.  \nSuch muons come from decays of mesons produced when ~8 TeV CR primaries hit the atmosphere, energies at which kaon production becomes important. Kaon decay produces a larger fraction of μ + than does pion decay, so an increased r=μ+/μ– would be seen.  \nE μ ,0 obtained from projection of μ back to surface along varying slant-depths of overburden.  \nPrevious best measurements of ratio are from L3+C, at a comparable depth to the MINOS ND.  \nMINOS ND ratio agrees with L3+C, but FD sees more positive muons at higher-energy (right) .  \nMeteorology and the Cosmic Ray Muon Rate  \nHadrons produced by primary cosmic ray interactions in the upper atmosphere either interact with the air or decay. Higher temperatures mean less density and more decays, thus a higher rate of high energy secondary cosmic ray muons seen deep underground.  \nUse twice-daily radiosonde flights from Intl. Falls, MN to get atmospheric temperature profile (newer analyses and SSW observations below use EWMCF interpolation model for higher completeness and accuracy)  ","cbCairjiFKspQz03","https://ap.wps.com/l/cbCairjiFKspQz03","pdf",2141339,"English","# The MINOS experiment and detectors\n## Far Detector vs Near Detector\n# Cosmic ray muons and charge ratio\n## Measurement strategy and results\n# Meteorology and muon rate\n## Temperature correlation and Sudden Stratospheric Warming\n# Cosmic ray shadows of the Sun and Moon","[{\"question\":\"What is the main physics goal of the MINOS experiment described here?\",\"answer\":\"The MINOS experiment uses a muon-neutrino beam and two layered detector systems to search for muon-neutrino disappearance, enabling tests of neutrino oscillations.\"},{\"question\":\"How is the cosmic-ray muon charge ratio measurement carried out?\",\"answer\":\"Muons are separated by charge using the MINOS magnetic field, using forward/reverse magnetic field configurations to cancel detector and field asymmetries and applying charge-selection cuts.\"},{\"question\":\"How does atmospheric temperature affect the underground muon rate in this study?\",\"answer\":\"Higher atmospheric temperatures reduce air density, increasing decay fractions of secondary particles and leading to a higher deep underground muon rate. The analysis uses an effective isothermal temperature and finds a correlation between changes in muon rate and temperature.\"}]","Cosmic Ray Studies with the MINOS Detectors - A.Habig, UMD | PDF",1792678474]