Neutrino Oscillation Phenomenology using atmospheric …Problem 29 • The neutrino oscillograms are...
Transcript of Neutrino Oscillation Phenomenology using atmospheric …Problem 29 • The neutrino oscillograms are...
Neutrino Oscillation Phenomenology using atmospheric neutrinos
Ioana Anghel1), Joshua Hignight2), Junting Huang3), Derek Rountre4)
1) Iowa State University/Argonne National Lab2) Stony Brook University3) University of Texas at Austin4) Virginia Tech
International Neutrino Summer School 2012 - Virginia Tech, July 20, 2012
(Group 9)
Problem 29
• The neutrino oscillograms are a useful way to explore the phenomenology of neutrino oscillations
• The goal: using the atmospheric neutrino oscillograms, determine the neutrinos mass hierarchy
• Approach:
- use the prob3++ package to make the oscillograms for different processes when neutrino
traverse the Earth
- compare the atmospheric neutrino oscillograms of the event rate for appearance channels
for different mass hierarchies
- by studying the resonances in the oscillograms for both neutrinos and anti-neutrinos, identify the
neutrinos mass hierarchy
⌫e
International Neutrino Summer School 2012 - July 20, 2012 2
Atmospheric neutrinos
ATMOSPHERIC NEUTRINOS
• The atmospheric neutrinos result from the interaction of cosmic rays with
atomic nuclei in the Earth atmosphere
• A shower of particles results from the interaction, the unstable particles
produce neutrinos when they decay
ATMOSPHERIC NEUTRINOS
• Neutrinos reach the Earth
at a certain Zenith angle (downward)✓ = 0✓ = ⇡ (upward)
3
Neutrino Oscillograms
4International Neutrino Summer School 2012 - July 20, 2012
• The neutrino oscillograms plot contours of equal oscillation probability in the neutrino energy -
zenith Earth angle
• Oscillograms - represented in (Energy, )✓
Probability
sin2(2✓13) = 0 sin2(2✓13) = 0.05 sin2(2✓13) = 0.1
P⌫µ!⌫e
International Neutrino Summer School 2012 - July 20, 2012 5
Y. Itow’s talk from Neutrino 2012
• The existence of a non-zero causes the appearance of high energy upward going neutrinos due to
the resonance effect✓13
Probability
sin2(2✓13) = 0 sin2(2✓13) = 0.05 sin2(2✓13) = 0.1
P⌫µ!⌫e
~ recently measured International Neutrino Summer School 2012 - July 20, 2012
Y. Itow’s talk from Neutrino 2012
• The existence of a non-zero causes the appearance of high energy upward going neutrinos due to
the resonance effect✓13
6
Resonances in Neutrino Oscillograms
7International Neutrino Summer School 2012 - July 20, 2012
• Resonances in oscillation probabilities occur when sin(2✓ij) = 1
• For different (i,j), the resonances occur at different energies. For resonances occur at energies
of ~ 4-10 GeV
• Resonance equation:
✓13
• The resonance condition:
where , GF is the Fermi constant and ne is the electron density in matter
• A > 0 for neutrinos, A < 0 for anti-neutrinos
• for normal mass hierarchy, for inverted mass hierarchy
-The resonance for neutrino energies from ~4-10 GeV occurs for neutrinos if normal hierarchy is correct while it would occur for anti-neutrinos if inverted-hierarchy is true. - By measuring the resonances for neutrino and anti-neutrinos in this energy range, one could distinguish normal from inverted hierarchy.
D. Indumathi and M. V. N. Murthy, "Question of hierarchy: Matter effects with atmospheric neutrinos and antineutrinos", Phys Rev D 71, 013001 (2005)
�23 > 0 �23 > 0
Neutrino Oscillations Parameters
8International Neutrino Summer School 2012 - July 20, 2012
• We used Prob3++ package to produce the neutrino oscillogramshttp://www.phy.duke.edu/~raw22/public/Prob3++/
• Oscillation parameters
sin2(2✓13) = 0.1
sin2(2✓12) = 0.825
sin2(2✓23) = 1.0
�CP = 0
�m122 = 7.9⇥ 10�5
�m232 = 2.5⇥ 10�3
- When neutrinos are traveling
in a vacuum, the oscillations are
seen directly in the oscillogram
for P
P in (Energy, ) plane for neutrinos in vacuum ✓
International Neutrino Summer School 2012 - July 20, 2012 9
normal Hierarchy
P in (Energy, ) plane for neutrinos in vacuum ✓
- Earth matter density is not zero, it varies with distance:
7/19/12 1:00 AM
Page 1 of 1http://upload.wikimedia.org/wikipedia/commons/e/ee/Earth-crust-cutaway-english.svg
Earth layer Distance (km) Density (g/cm3)
Crust 0-35 2.2-2.9
Mantle 35-2890 3.4-5.6
Core 2890-6378 9.9-13.1
International Neutrino Summer School 2012 - July 20, 2012 10
normal Hierarchy
- When neutrinos are traveling
in vacuum, the oscillations are
seen directly in the oscillogram
for P
Vacuum
Earth density
P comparison for vacuum / Earth density
11
normal Hierarchy
- the matter effect is seen for a
non 0 zenith angle, for neutrinos
travelling distance d > 1000 km
Vacuum
Earth density
P comparison for vacuum / Earth density
12
normal Hierarchy
Normal Mass Hierarchy
P (E, ) for different mass hierarchies - neutrinos✓
• For energies of a few GeV, is large, while is quite low for normal mass hierarchy P⌫µ!⌫e P⌫e!⌫e
International Neutrino Summer School 2012 - July 20, 2012 13
Normal Mass Hierarchy
Inverted Mass Hierarchy
• Both and
are close to 0 at E ~ few GeV
P⌫µ!⌫eP⌫e!⌫e
14
P (E, ) for different mass hierarchies - neutrinos✓
Normal Mass Hierarchy
Inverted Mass Hierarchy
• The case is reversed for
electron anti-neutrino channels
( e.g. > 0 for
inverted mass hierarchy )
P⌫µ!⌫e
15
P (E, ) for different mass hierarchies - anti-neutrinos✓
From Probability to Event Rate
International Neutrino Summer School 2012 - July 20, 2012 16
From Probability to Event Rate
(s−1m
−2GeV
−1Sr
−1)
The number of event in the detector can be written as
Δ N=−N σ nL
=−(∫FL2dEdΩdT )σ nL
=−(∫FdEdΩdT )σ (n L3)
Total number of target in detector
L: detector size
σ: cross section n: the number of target per unit volume
F: Azimuth angle averaged
flux
(Honda flux table)
K. Hagiwara et al., Phys. Rev. D 66 (Review of Particle Physics 2002)
http://www.icrr.u-tokyo.ac.jp/~mhonda/
An EstimationFor a 50 kiloton water Cerenkov detector (Super K),
Event Rate =(∫FdEdΩdT )σ (nL3)=0.11 per year
nL3=3×10
33
F∼1 s−1
m−2
GeV−1
Sr−1
(for cosθ=−0.7∼−0.8, E=6.3GeV)
∫dE∼2GeV
∫dΩ=∫dcosθd φ∼0.1×π=0.628
∫dT=1 year∼3×107s
σ=10−42
m2
Total # of nuclei
Flux
Resonance width
Solid angle
1 year data
Cross section
With those numbers, one has
An Estimation
International Neutrino Summer School 2012 - July 20, 2012 17
An EstimationFor a 50 kiloton water Cerenkov detector (Super K),
Event Rate =(∫FdEdΩdT )σ (nL3)=0.27 per year
nL3=3×10
33
F∼1 s−1
m−2
GeV−1
Sr−1
(for cosθ=−0.7∼−0.8, E=6.3GeV)
∫dE∼2GeV
∫dΩ=∫dcosθd φ∼0.3×2π=1.9
∫dT=1 year∼3×107s
σ∼0.8×10−42
m2for ν
(2 to 3 times smaller for ν̄)
Total # of nuclei
Flux
Resonance width
Solid angle
1 year data
Cross section
With those numbers, one has
Flux (E, ) Distribution✓
• The atmospheric neutrino flux for SuperK is relatively high for low energies (~102 MeV) and
decreases while the zenith angle approaches 0 or ⇡• For neutrinos with energies ~ GeV, the flux is ~ 10-3.
International Neutrino Summer School 2012 - July 20, 2012 18
Normal Mass Hierarchy
Event Rate (E, ) for different mass hierarchies✓
• The event rate for neutrinos with energies ~ GeV is
very low (~ 10-2) compared to low energies neutrinos.
International Neutrino Summer School 2012 - July 20, 2012 19
5Normal Mass Hierarchy
Event Rate (E, ) for different mass hierarchies✓
International Neutrino Summer School 2012 - July 20, 2012 20
Normal Mass Hierarchy
Inverted Mass Hierarchy
Event Rate (E, ) for different mass hierarchies✓
21
• At resonance, there is an
excess in the event rate for
normal wrt inverted
hierarchies
• After one year of running,
integrating over the entire
area of resonance, we can
observe ~ 1 event
5
5
Normal Mass Hierarchy
Inverted Mass Hierarchy
Event Rate (E, ) for different mass hierarchies✓
22
• For anti-neutrinos, the
excess in the event rate is
observed for the inverted
hierarchy
5
5
Differences in the Event Rate for different hierarchies
• Without identifying between neutrinos and anti-neutrinos, the
differences between the mass hierarchies
is quite low.
• To compute the event rates we need to
use the cross sections for neutrinos and
anti-neutrinos (2-3 lower than neutrinos)
• Need for a much higher statistics !!!
23
Normal H
Inverted H
5
5
Differences in the Event Rate for different hierarchies
24
Normal H
Inverted H • Separating neutrinos from anti-neutrinos, the
differences between the
mass hierarchies are larger.
5
5
5
5
25International Neutrino Summer School 2012 - July 20, 2012
• Our calculations are slightly better than the real world
• In the current configuration of SuperK many years of running are necessary to get the needed statistics
• What would be necessary?
- higher statistics- charge separation detector- neutrino beam
Requirements for identifying mass hierarchy using oscillograms
• Our calculations are slightly better than the real world
• In the current configuration of SuperK many years of running are necessary to get the needed statistics
• What would be necessary?
- higher statistics- charge separation detector- neutrino beam
Normal Mass Hierarchy
Inverted Mass HierarchyMuon Neutrino
beam
Requirements for identifying mass hierarchy using oscillograms
55 26
Requirements for identifying mass hierarchy using oscillograms
4
• Our calculations are slightly better than the real world
• In the current configuration of SuperK many years of running are necessary to get the needed statistics
• What would be necessary?
- higher statistics- charge separation detector- neutrino beam
Muon anti-
Neutrino beam
Normal Mass Hierarchy
Inverted Mass Hierarchy
5
5
5
5
5
5
27
Back-up
36° 20' 24'' North , 137° 19' 48'' East
SuperK
54° 20' 24'' South , 43° 19' 48'' West
29
30
sin2(2✓13) = 0.08 sin2(2✓13) = 0.1 sin2(2✓13) = 0.12
Probability in (Energy, ) plane✓
31
sin2(2✓13) = 0.1 sin2(2✓13) = 0.12sin2(2✓13) = 0.08
Probability in (Energy, ) plane✓
Mass Hierarchy Effect on the Event Rate
32
Normal Mass Hierarchy
Inverted Mass Hierarchy
Mass Hierarchy Effect on the Event Rate
33
Normal Mass Hierarchy
Inverted Mass Hierarchy
34
�CP = 0 �CP = ⇧/4 �CP = ⇧/2Normal H
Inverted H
Event Rate (E, ) for different mass hierarchies✓
35
�CP = ⇧/2�CP = ⇧/4�CP = 0Normal H
Inverted H
Event Rate (E, ) for different mass hierarchies✓