Neutrinos Ghosts of the Universe Don Lincoln Fermilab

Neutrinos: Ghosts of the Universe Don Lincoln Fermilab f

Beauty in the Universe

Much is explained by quarks and electrons. But there remains the neutrino. . . ~109 /proton!!

b decay n e o neutr n proto Observed d Sin gl e. V e u l a Re a lit y

e oton n on r t u e pr December 4, 1930 b decay Dear radioactive ladies and gentlemen, . . . I have hit upon a ‘desperate remedy’ to save. . . the law of conservation of energy. Namely the possibility that there exists in the nuclei electrically neutral particles, that I call neutrons. . . I agree that my remedy could seem incredible. . . but only the one who dare can win. . . Unfortunately I cannot appear in person, since I am indispensable at a ball here in Zurich. Your humble servant W. Pauli Note: this was before the discovery of the real neutron

Project Poltergeist 1956 Signal 2 g, then several g ~few ms later Reines neutrino g Cowan Cd Experiment attempted at Hanford in 1953, too much background. Repeated at Savannah River in 1955. [Flux: 1013 neutrinos/(cm 2 s)] e+ n p+ g H 2 O + Cd. Cl 2

Neutrino Facts Neutrino from Enrico Fermi for “Little neutral one” flux on Earth from Sun 6. 5× 1014/(m 2 s) <E> ~ 0. 3 Me. V Neutrino from sun will pass through 5 LY of solid lead, with 50% chance of interacting Average number of solar neutrinos interacting in a person per year 30! 1 with ‘real energy’

Neutrinos in Art Cosmic Gall Neutrinos, they are very small. They have no charge and have no mass And do not interact at all. The earth is just a silly ball To them, through which they simply pass, Like dustmaids down a drafty hall Or photons through a sheet of glass. Neo-Swing They snub the most exquisite gas, Ignore the most substantial wall, Cold-shoulder steel and sounding brass, Insult the stallion in his stall. And, scorning barriers of class, Infiltrate you and me! Like tall And painless guillotines, they fall Down through our heads into the grass. At night, they enter at Nepal And pierce the lover and his lass From underneath the bed—you call It wonderful; I call it crass. John Updike Telephone Poles and Other Poems, 1963 Seattle Rock Band

More than one kind of neutrino? p+ p± m± Tons of steel Date: 1962 Intent: Measure weak force at high energies Expectation: Since neutrinos are created with muons and electrons, the neutrino beam should create both electrons and muons in the detector. Result: No electrons produced, only muons Conclusion: There must be two kinds of neutrinos. Detector Mel Schwartz

What Good are Neutrinos? e h t l ee f y l on e. s o trin k forc u e N wea Over simplified u u d Other probes of nucleon structure have to beat their way through the mess that is a real proton. Multiple interactions means messy interpretation. Neutrinos interact at most once, so the collision is more easily understood.

Nucleon Structure Z u u d 18 m m W u u 28 m d

Fraction of momentum carried by parton Probability Distribution “Expectation” Nucleon Structure of the proton can be determined by scattering neutrinos (or other probe particles) into hydrogen target

Typical Experiment Need lots of mass to force a neutrino to interact. Beam-based experiments typically have weight of ~1000 tons

Neutrinos show number of generations At LEP A Z can also decay into neutrino pairs. The width of the mass distribution of the Z boson is sensitive to the total number of neutrino generations into which it can decay. Obvious Conclusion: There are 3 generations Cautious Conclusion: There are only three flavors of low-mass neutrinos into which a Z can decay.

In the 1993 episode of Star Trek: Deep Space 9 called “Rivals” neutrinos were a plot twist. Star Trek • Quark was losing money. • Jadzia noticed that 98% of neutrinos were spinning one way. • She explains half should spin each way. ! h • The crew locates ‘luck changing’ machines. a H

Solar neutrinos p + p d + e + + e 8 B 8 Be + e+ + e Uranium and Thorium in the Earth’s crust decay about 15 TW of energy. Neutrino flux on Earth’s surface (from Earth) ~ 5× 1010 s-1 m-2 Sun emits e 2× 1038 s-1 Neutrino Sources A 5 -10 GW reactor complex has a neutrino flux of ~1020 s-1 Neutrinos from cosmic rays ~100 m-2 s-1

Homestake Gold Mine 100, 000 gallons of cleaning fluid C 2 Cl 4 Expected 1. 5 interactions per day Measured 0. 5 interactions per day Sensitive to 8 B solar neutrinos only e + 37 Cl e- + 37 Ar Ray Davis John Bahcall 19 ! 8 6

SAGE Soviet-American Gallium Experiment + 71 Ge + e. Sensitive to pp fusion in sun. 71 Ga 50 metric tons of Gallium They extract a few tens of atoms of Germanium Measured: 77 6 3 SNU Predicted: 123 + 9 -7 SNU

Solar Neutrino Summary Different experiments are sensitive to different solar processes. But all experiments show a marked deficit of electron neutrinos. Could reflect ignorance of how the sun works. Except. . .

In the early 1980 s, two experiments (IMB Irvine. Michigan-Brookhaven) and (Kamiokande) were built to look for proton decay. Accidental Evidence None detected. Proton lifetime > 1033 years. SN 1987 A 7: 36 neutrinos observed 9: 30 amateur astronomer observes Tarantula Nebula in LMC. Nothing unusual. 10: 30 LMC photographed, SN 1987 A observed. Simulated Event ~3 hours for shock wave to hit surface.

If proton decay goes as Signal is ring in detector. Anything that can make a ring is background. Background Becomes Signal Knowledge of detector response problematic. Compensate by double ratio: Expected average ratio R = 1. In cosmic ray showers, expect 2 m for each e

Hmmmm. . .

Hmmmm. . .

Quantum Cobwebs Remember that information on a state is encoded in a wave function. Remember that you can express the wave function in any orthogonal basis (coordinate system). Under the electromagnetic force, the electrically-charged object (say an electron) is an eigenstate of mass and electrical charge. Under the weak force, the weak-charged object (say an neutrino) is not both an eigenstate of mass and weak charge. Crucial insight Weak charge = k 1 (mass 1) + k 2 (mass 2) k 21 + k 22 = 1

m 2 Massive Neutrinos Math m 2 e e q 1 m 2 e 1 1

Massive Neutrinos Math Mass Basis Weak Charge Basis Important!

Massive Neutrinos Math Substitute weak basis Time dependent Schrodinger equation

Massive Neutrinos Math Initial conditions Evaluate Reasonable approximations

Massive Neutrinos Math

Super Kamiokande

Super Kamiokande 11 stories high 1, 000 meters underground 50, 000 tons of water 22, 500 tons fiducial volume 11, 200 photomultipliers 0. 5 meter photomultiplier diameter Abandoned zinc mine

Super Kamiokande Discovery Announcement June 5, 1998 Gist: “There are fewer upcoming muon neutrinos than expected from down-going neutrino flux. Data consistent with neutrino oscillations. ”

SNO Sudbury Neutrino Observatory In Sudbury, Ontario • Cerenkov detector • Heavy water (can do solar model independent measurements) • 6800 feet underground • 9600 PMTs

Charged interactions convert neutron to proton. Sensitive only to e. 30 events/day Neutral interactions disassociate deuteron into neutron and proton. Sensitive to e , m, t. 30 events/day SNO Physics and Results Announcement: June 18, 2001 Comparison of SNO results with Super K Electron scattering indicates that the mostly sensitive to e, neutrino flux from the with small contribution sun contains muon from m , t. neutrinos, supporting 3 events/day neutrino oscillations.

So What Does It Mean? • Data is consistent with neutrino oscillations. This can be accommodated, but not explained, by known physics. • Data from solar and atmospheric neutrinos is consistent with ~ m 2 m 3 m 1 • Solar electron neutrinos disappear and reappear into muon neutrinos • Atmospheric muon neutrinos disappear and reappear into tau neutrinos

Cosmological Implications of Neutrinos ~ 330 /cm 3 (from Big Bang) <E> ~ 0. 0004 e. V (from Big Bang) Runiverse ~ 1010 lightyears Vuniverse ~ 4× 1084 cm 3 If neutrinos were massive objects, they could contribute significantly to the mass of the universe. N ~ 1087 E (total) ~ 4× 1083 e. V M (equivalent) ~ 7× 1047 kg Muniverse(visible) ~ 4× 1052 kg Are Neutrinos Massless? 0. 1% < M < 18%

At 11: 00, November 12, 2001, about 60% of the phototubes used in the Super-K detector imploded within a few seconds. $21, 000 damage We will rebuild the detector. There is no question. - Yoji Totsuka Director, Super-K Observatory Osama bin Laden on Super-K Disaster: Neutrinos are “. . . an abomination on the face of god. . . ” and the search for neutrino mixing is: “. . . idolatry, which will be smashed beneath the fist of righteousness. . . ” Disaster Strikes!

LSND Liquid Scintillator Neutrino Detector 1996 Reports conversions of nm to ne. Other experiments do not confirm. Outstanding Questions Highly controversial result. If true, significant theoretical work needs doing. e n o o i. B te n i fu M re s ’ or b ila irm 002 rm nf r 2 e F co me to um S

Neutrino Summary • They interact with ordinary matter very weakly. • Their behavior is highly complex and will need new physics to explain it. • Many experiments not mentioned here are ongoing to unravel this rich behavior.

www-d 0. fnal. gov/~lucifer/Power. Point/Neutrinos. ppt