Neutrino
Physics & Experiment
Neutrino physics has had an interesting history. In 1930
Pauli postulated the existence of the (electron) neutrino, in
1956 this was confirmed by
Reines and Cowan using a nuclear
reactor source of antineutrinos. In 1962, a second distinct
(muon) neutrino was shown to exist in a BNL experiment. For
that discovery Nobel Prize was awarded to Lederman,
Schwartz and Steinberger. In 1995, the third, (tau) neutrino was
detected at FNAL. In parallel, Ray Davis' studies of solar
neutrinos confirmed understanding of stellar dynamics modulo
a 2/3 flux deficit that later was recognized as a result of
neutrino oscillations among the three flavors of neutrinos.
properties of those oscillations were further unveiled with
followup solar, atmospheric, reactor and accelerator neutrino
studies . The discovery of oscillations, detection of 19
neutrino events from supernova 1987a by the old IMB and
Kamiokande water cerenkov detectors confirmed the theory of
supernova explosions. The WMAP experiment has started to see
imprints of neutrino mass effects on the cosmic microwave
background radiation left from the Big Bang.
Introduction
An intense neutrino facility allows probing of the
neutrino mixing angles, mass hierarchy, and leptonic CP
violation. Physics potential, for making precision
measurements of all neutrino oscillation parameters. using a
wide band nu_µ beam from BNL , to a VLB (very long baseline)
2540 km baseline (with 0.5 megaton) detector at Homestake
Mine in South Dakota was our first study. Potentials of
intense neutrino beams from BNL (FNAL) to Long Baseline
Detectors at Homestake (SD), Henderson (Co) and Cascades (WA)
were studied. Large Detectors located in a low background
underground environment(s) would provide additional physics
capabilities for proton decay and continuous observation of
natural sources of neutrinos such as supernova. HOMESTAKE is
the selected DUSEL Site, Detector R & D is underway,and
our neutrino to VLB simulation(s) are illustrated. Left Tabs
provide additional information on Long Baseline (LBNE), Reactor
(DAYA BAY) and Solar
Neutrino (Nu) Experiments etc.
* With "Firefox Browser"
you can see this page with (rotating) plots of
parameters variations, click |HERE|
Zohreh Parsa
parsa@bnl.gov
www.neutrino.bnl.gov
 
Top Figure shows variation of parameter(s) e.g L (Baseline) distance
from neutrino source to a detector site.
Lower Plot shows CP Phase Variations, in above Probability vs Energy plot(s).
Neutrino
(alias Neutrinos) page, updated 1999 - June 2011, Dr. Z.
Parsa, Physicist; Address: Physics Department 510A, Brookhaven
National Lab, Upton, New York 11973-5000, USA
Past web assist appreciated. Privacy and Security Notice
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BNL, FNAL and 3 possible DUSEL
Detector Sites, Homestake (SD), Henderson (CO), cascades(WA).
DUSEL selected site is
the Homestake Mine in South Dakota, a
distance of 2540 km
from BNL and close to 1300 km from
FNAL. |
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Super Kamiokande, a Water Cerenkov Detector
Ribon Cutting with Dr. Al
Mann at the
HOMESTAKE, Sanford Underground Laboratory
Drs. Z. Parsa, W. Marciano & R. Wilson in Henderson (a
DUSEL possible) UNDERGROUND Lab site in Colorodo.
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