Main injector neutrino oscillation search (MINOS) was aparticle physics experiment designed to study the phenomena ofneutrino oscillations, first discovered by aSuper-Kamiokande (Super-K) experiment in 1998.Neutrinos produced by theNuMI ("Neutrinos at Main Injector")beamline atFermilab nearChicago are observed at two detectors, one very close to where the beam is produced (thenear detector), and another much larger detector 735 km away in northernMinnesota (thefar detector).
The MINOS experiment started detecting neutrinos from the NuMI beam in February 2005. On 30 March 2006, the MINOS collaboration announced that the analysis of the initial data, collected in 2005, is consistent with neutrino oscillations, with the oscillation parameters which are consistent with Super-K measurements.[1]MINOS received the last neutrinos from the NUMI beam line at midnight on 30 April 2012.[2][3] It was upgraded toMINOS+ which started taking data in 2013.[4] The experiment was shut down on June 29, 2016, and the far detector has been dismantled and removed. It was moved to Puerto Vallarta, Jalisco in Mexico.[5]
There are two detectors in the experiment.
Both MINOS detectors aresteel-scintillator samplingcalorimeters made out of alternating planes of magnetized steel andplastic scintillators. Themagnetic field causes the path of amuon produced in amuon neutrinointeraction to bend, making it possible to distinguish interactions with neutrinos from those with antineutrinos. This feature of the MINOS detectors allows MINOS to search forCPT-violation with atmospheric neutrinos and anti-neutrinos.
To produce theNuMIbeamline, 120 GeVMain Injector proton pulses hit a water-cooledgraphite target. The resulting interactions of protons with the target material producepions andkaons, which are focused by a system ofmagnetic horns. The neutrinos from subsequent decays of pions and kaons form theneutrino beam. Most of these are muon neutrinos, with a smallelectron neutrino contamination. Neutrino interactions in the near detector are used to measure the initial neutrinoflux and energy spectrum. Because they are weakly interacting and therefore usually pass through matter, the vast majority of the neutrinos travel through the near detector and the 734 km of rock, then through the far detector and off into space. On the way toward Soudan, about 20% of the muon neutrinos oscillate into otherflavors.
MINOS measures the difference in neutrino beam composition and energy distribution in the near and far detectors with the aim of producing precision measurements of the neutrino squared mass difference andmixing angle. In addition, MINOS looks for the appearance of electron neutrinos in the far detector, and will either measure or set a limit on the oscillation probability of muon neutrinos into electron neutrinos.
On 29 July 2006, the MINOS collaboration published a paper giving their initial measurements of oscillation parameters as judged from muon neutrino disappearance. These are:Δm2
23 =2.74+0.44
−0.26 × 10−3 eV2/c4 andsin2(2θ23) > 0.87 (68% confidence limit).[8][9]
In 2008, MINOS released a further result using over twice the previous data (3.36×1020 protons-on-target; this includes the first data set). This is the most precise measurement of Δm2. The results are:Δm2
23 =2.43+0.13
−0.13 × 10−3 eV2/c4 andsin2(2θ23) > 0.90 (90% confidence limit).[10]
In 2011, the above results were updated again, using a more than double data sample (exposure of 7.25×1020 protons on target) and improved analysis methodology. The results are:Δm2
23 =2.32+0.12
−0.08 × 10−3 eV2/c4 andsin2(2θ23) > 0.90 (90% confidence limit).[11]
In 2010 and 2011, MINOS reported results according to which there is a difference in the disappearance and consequently the masses between antineutrinos and neutrinos, which would violateCPT symmetry.[12][13][14]However, after additional data were evaluated in 2012, MINOS reported that this gap has closed and no excess is there any more.[15][16]
Cosmic ray results from the MINOS far detector have shown that there is a strong correlation between high energy cosmic rays measured and the temperature of thestratosphere. This is the first time, daily variations in secondary cosmic rays from an underground muon detector are shown to be associated with planetary–scale meteorological phenomena in the stratosphere such as thesudden stratospheric warming[17] as well as the change in seasons.[18] The MINOS far detector is also able to observe a reduction in cosmic rays caused by theSun and theMoon.[19]
In 2007, an experiment with the MINOS detectors found the speed of3 GeV neutrinos to be1.000051(29) c at 68% confidence level, and at 99% confidence level a range between0.999976 c to1.000126 c. The central value was higher than the speed of light; however, the uncertainty was great enough that the result also did not rule out speeds less than or equal to light at this high confidence level.[20][21]
After the detectors for the project were upgraded in 2012, MINOS corrected their initial result and found agreement with the speed of light, with the difference in the arrival times of −0.0006% (±0.0012%) between neutrinos and light. Further measurements are going to be conducted.[22]
That group found, although with less precision, that the neutrino speeds were consistent with the speed of light.
47°49′12″N92°14′30″W / 47.82000°N 92.24167°W /47.82000; -92.24167
