V. A. Naumov Physics of Atmospheric Neutrinos Abstract The lecture reviews the physics of neutrino production in the atmosphere, the detection methods, and the results obtained with large underground neutrino detectors. Contents of the lecture. 1. Introduction. The role of atmospheric neutrinos (AN) in astroparticle physics. 2. Mechanisms and the main features of neutrino production in the earth's atmosphere at low, intermediate, and high energies. 3. A short review of calculational methods. 4. Sketch of numerical results. Comparison between different models and analysis of uncertainties. 5. Verification of the AN flux calculations with the cosmic-ray secondaries in the atmosphere and ground level. 6. Underground muons as a tool for the AN flux normalization. 7. Detection methods. Description of the largest underground neutrino detectors. Neutrino-induced events classification. 8. Search for neutrino oscillations in underground experiments. 9. Results from the detectors Kamiokande, IMB, NUSEX, Frejus, SOUDAN 2, MACRO, and Super-Kamiokande. Interpretation of the data in terms of neutrino oscillations. 10. Other explanations (proton decay, neutrino decay, FCNC, neutron background, etc). 11. Conclusions.
This document is posted to help you gain knowledge. Please leave a comment to let me know what you think about it! Share it to your friends and learn new things together.
The lecture reviews the physics of neutrino production in the atmosphere, the detection methods, and the results obtained with large underground neutrino detectors.
Contents of the lecture.
1. Introduction. The role of atmospheric neutrinos (AN) in astroparticle physics. 2. Mechanisms and the main features of neutrino production in the earth's atmosphere at low, intermediate, and high energies. 3. A short review of calculational methods. 4. Sketch of numerical results. Comparison between different models and analysis of uncertainties. 5. Verification of the AN flux calculations with the cosmic-ray secondaries in the atmosphere and ground level. 6. Underground muons as a tool for the AN flux normalization. 7. Detection methods. Description of the largest underground neutrino detectors. Neutrino-induced events classification. 8. Search for neutrino oscillations in underground experiments. 9. Results from the detectors Kamiokande, IMB, NUSEX, Frejus, SOUDAN 2, MACRO, and Super-Kamiokande. Interpretation of the data in terms of neutrino oscillations.10. Other explanations (proton decay, neutrino decay, FCNC, neutron background, etc).11. Conclusions.
file:///G|/Works/BSFPh98/Lecture/Misc/Abstract%20to%20Lecture%20at%20KIAS.txt10/10/2005 12:28:48 AM
10-1
1
10
102
10 -3 10 -2 10 -1 1sin2 2
∆m2
[eV
2 ]
BNL E776
LSND93-97
CCFR
BUGEY
KARMEN2Feb.97-Apr.9890 % CL exclusion
KARMEN2Feb.97-Apr.98sensitivity
0.5 0.0 0.5 1φ(7Be) / φ(7Be)SSM
0.0
0.5
1.0φ(
8 B)
/ φ(8 B
) SS
MMonte Carlo SSMsTL SSMLow ZLow opacityWIMPLarge S11Small S 34Large S33Mixing modelsDarShaviv modelCummingHaxton model
T C power law
BP SSM
Smaller S17Combined fit90, 95, 99% C.L.
Energy (GeV/particle)
m-2 s
sr
(GeV
/par
ticle
)-1
-11.
75 [
]
E
dF/
dE2.
75
10 10 10 10 10 10 10 10 103 4 5 6 7 8 9 10 11
4
5
6
10
10
10
103
Grigorov et al.Ichimura et al.JACEETien ShanNorikura
Tibet AS EAS-TOPDiceTunkaAkeno
SUGARHaverah ParkYakutskFly’s EyeAGASA
"All-particle" spectrumof primary cosmic rays
direct data
γ
these two pointsare senseless
-1-1
(GeV
/nuc
leon
) ]
[ms
srdF
/dE
-1
-24
Kinetic Energy [GeV/nucleon]10-1 100 101 102 10310-4
Selected predictions for high-energy neutrino fluxes (from P. Gondolo, Proc. of the 4th SFB-375 Ringberg Workshop on Neutrino Astrophysics, Oct. 20-24, 1997)
LVDData converted to standard rockData for Gran Sasso rock (x 10-1)
π,K-muonsπ,K-muons + Iµ
ν
π,K-muons + Iµν + PM (RQPM)
π,K-muons + Iµν + PM (VFGS)
Iµν =2.98x10-13 cm-2s-1sr-1
Inte
nsity
( c
m-2
s-1sr
-1 )
Depth (km w.e.)
Muo
n
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1
0 5 10 15 20 25 30 35 40
BEBC (1979-1982)
BNL (1980-1981)
CRS (1980-1981)
FNAL (1977-1983)
GGM (1979-1981)
IHEP-ITEP (1979-1983) SKAT (1979)
IHEP-JINR (1995)
ν N
ν– N
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1
50 75 100 125 150 175 200
BEBC (1979-1982)
FNAL (1977-1983) CCFRR (1984) 20-200 GeV average
ν N
ν N
IHEP-ITEP (1979-1983)
Eν (GeV)225
Eν (GeV)
σC
Cto
t10
-38
Eν
(cm
/G
eV )
2/ –
Through-going muons
Stopping muons
Kamiokande multi-GeV
Contained events ( x1/10 )
10 10 10 10 10 10 10-1 0 1 2 3 4 5
E (GeV)
E d
N /d
En
n n
nM
uon-
neut
rino
resp
onse
(Bar
tol,
11/1
1/19
96)
50
45
40
35
30
25
20
15
10
5
0
Distance
under ground
1.6 km
SUPERKAMIOKANDE DETECTORCatching NeutrinosAbout once every 90 minutes, a neutrino interacts in the detectorchamber, generating Cherenkov radiation. This optical equivalent ofa sonic boom creates a cone of light that is registered on thephotomultipliers that line the tank. Characteristic ring patterns tellphysicists what kind of neutrinos interacted and in which directionthey were headed.
The light isdetected byphoto sensorsthat line thetank, andtranslated into adigital image.
Electronicstrailers
Controlroom
Accesstunnel(2 km)
12.5 million gallontank of ultra-purewater
Mt. Ikena Yama
Mountains filter out other signalsthat mask neutrino detection.
A few neutrinos interactwithin the huge tank of superpure water, generating acone of light.