resonant neutrino self-interaction with u(1)l -l model...resonant neutrino self-interaction with...
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![Page 1: Resonant Neutrino Self-Interaction with U(1)L -L Model...Resonant Neutrino Self-Interaction with U(1) Lμ-Lτ Model AYUKI KAMADA (UC Riverside) in collaboration with Hai-bo Yu (UCR)](https://reader033.vdocuments.site/reader033/viewer/2022041903/5e61ba976527ad31925df309/html5/thumbnails/1.jpg)
Resonant Neutrino Self-Interaction
with U(1)Lμ-Lτ Model
AYUKI KAMADA (UC Riverside) in collaboration with Hai-bo Yu (UCR)
@第28回宇宙ニュートリノ研究会
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“Dip” in IceCube
Good fit w/ ϕ(Ε)∝E-2
Missing events
at subPeV M. Aartsen et al. 2014
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Possible InterpretationSources w/ ϕ(Ε)∝E-2
• Astrophysical (GRB, SNR)• Cosmogenic (pp, pγ…)• New Physics (DM decay, annihilation)
Origins w/ dip• Statistical fluctuation
-a few events expected (2σ consistent)• New Physics (neutrino interactions)
This talk
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How does neutrino self-interaction work?
𝛎p~PeV
𝛎
k~10-4 eV
𝛎
𝛎
p’~p/2
k’~p/2
High energy neutrino
cosmic neutrinobackground (C𝜈Β)
High energy neutrino deposits their energy in cosmic neutrino background
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Exclusive for subPeVOnly subPeV neutrinos interact effectively
achieved by Breit-Wigner Resonance
cosθ: injection angleTypically m𝜈 ~ 0.1 eV
>> k~10-4 eV~10 MeV
𝜈𝜈 -> Z’ -> 𝜈𝜈
mZ0 =p2m⌫p
m2Z0 = 2p(
pk2 +m2
⌫ � k cos ✓)
10 MeV mediator implied!!
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Well-motivated model
Gauging (muon number - tau number) 𝜈μ(+1), 𝜈τ(-1)… anti-particles(opposite sign)
couple with Z’-boson (mZ’~10MeV!!)
Advantages• Anomaly-free (well-defined theory)• natural explanation of maximal mixing
for atmospheric neutrino θ23~π/4• No experimental difficulty
unlike U(1)Le-Lμ, U(1)Le-Lτ
(e.g. beam-dump experiment)
U(1)Lμ-Lτ
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Muon g-2
aμ=(g-2)/2~0.001
Measured muon anomalous magnetic moment (g-2) deviates from standard model prediction
𝛥aμ(exp)=aμ(exp) - aμ(SM)=(42.6±16.5)×10-10
Z’-boson exchange contribution
�a
Z0
µ =g
0 2
8⇡2
Z 1
0dx
2m2µx
2(1� x)
x
2m
2µ + (1� x)m2
Z0
Gauge coupling of g’~10-4 can fill the gap!!
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Optical depth
e⌧s(z) = 18⇣(3)T 3⌫,0(1 + z)3
1
H(z)m2Z0
�Z0
mZ0
' 1
✓g0
2.5⇥ 10�5
◆2
C𝜈Β number density
Streaming Length
Cross section
Gauge coupling of g’~10-4 is also sufficient to explain dip in IceCube!!
T. Araki et al. 2014
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𝛎Β
𝛎Β
Is this brilliant story true?𝛎e
𝛎Β
𝛎μ
𝛎τ
𝛎e 𝛎Β
𝛎
𝛎
𝛎
𝛎
𝜈e’s can reach us without losing energy flavored (<->flavor-blind)
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Neutrino oscillation I𝛎e
Starting with
IceCube
w/o oscillation𝛎Β
𝛎Β 𝛎e
Source 𝛎e
𝛎e 𝛎μ
𝛎τ
Neutrinos change their flavors during
oscillations
(c) IceCube
(c) NASA
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Neutrino oscillation II𝛎e
Starting with
IceCube
w/ oscillation𝛎Β
𝛎Β 𝛎e
Source 𝛎e
𝛎μ
𝛎τ
𝛎Β
𝛎Β
Even starting with 𝜈e’s, only a part of 𝜈’s can reach us
(c) NASA
(c) IceCube
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Neutrino oscillation IV
P '
2
40.30 0.13 0.120.13 0.06 0.050.12 0.05 0.04
3
5
+e�e⌧s(zs)/2
2
40.07 �0.05 �0.03�0.05 0.03 0.02�0.03 0.02 0.01
3
5
+e�e⌧s(zs)
2
40.18 0.15 0.120.15 0.29 0.310.12 0.31 0.35
3
5
Starting with
Probability matrix𝛎e 𝛎μ 𝛎τ End up with
𝛎e
𝛎μ
𝛎τ
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Predictions and Prospectspp interaction(�⌫e ,�⌫µ ,�⌫⌧ ) ' (1, 2, 0)
@ IceCube (1/3 survived)(0.56, 0.25, 0.22)
z=zs z=0 Accumulated date can
distinguishflavored modelfrom
flavor-blindmodel
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Cosmological/Astrophysical Aspects
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Cosmology of 10 MeV Z’-boson I
inverse decay pair creation
decay pair annihilationTwo relevant processes
Dominant @ high-T @ low-TTcrit ' 100GeV ⇥
✓10�4
g0
◆⇥
⇣ mZ0
10MeV
⌘
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Cosmic history w/ Z’
T~10 MeV T~0.1 MeVT~1 MeV
e 𝜈 𝛾
𝜈
e 𝛾 𝛾
BBNe-e+ annihilation𝜈’s decoupling
Ζ᾽
Ζ᾽
μ/π’s decay
Important question: When is Z’ decays?
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Decoupling of Z’ III
T~10 MeV T~0.1 MeVT~1 MeV
e 𝜈 𝛾
𝜈
e 𝛾
BBNe-e+ annihilation𝜈’s decoupling
Ζ᾽
Ζ᾽
μ/π’s decay
Z’ decays in-between
heated 𝜈’s change the expansion ratespoil success of SM in BBN
𝛾
mZ’> 6.3 MeV
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Core Collapse SNCore
Produced 𝜈’s can not escape from proto-neutron star
Neutrino sphere
Random walk
R = λ√N
T~8 MeVR~15 km
mean free path # of collisions
N=t/λλ~4 mt~10s
It takes
until escape
λ
𝛎
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SN1987AThis 10s determines the duration of neutrino cooling
M. Nakahata 2007
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Core Collapse SN w/ Z’Core
Same story for 𝝂e, but not for 𝝂μ 𝝂τ
Neutrino sphere
𝝂e
T~8 MeVR~15 km
inverse decay
decay𝛎e𝛎μ
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Diffusion time w/ Z’
Diffusion time t~105s >> 10s (SN1987A)Mean free path λ~0.01cm
For g’~10-4 (good for Muon g-2, IceCube dip)
Notion• More detailed study needed to conclude…• Some additional cooling mechanism of core
(e.g. axion, hidden photons)
Only 𝝂e’s contribute to SN cooling
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Prediction
𝛎e𝛎μ
SN
Super Kamiokande
𝛎τOnly 𝝂e’s are emitted from SN
Important hint ofthis scenario
(c) NASA
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Summary