Probing non-unitarity with atmospheric neutrinos Hisakazu Minakata - - PowerPoint PPT Presentation

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Probing non-unitarity with atmospheric neutrinos Hisakazu Minakata - - PowerPoint PPT Presentation

Dec 08, 2022 374 likes •722 views

Probing non-unitarity with atmospheric neutrinos Hisakazu Minakata IFT UAM/CSIC, Chee Sheng Fong, HM, Hiroshi Nunokawa, Madrid arXiv:1609.08623, 1712.02798 We see things converge T2K see more and more preference of ~ 3 /2 T2K II

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Probing non-unitarity with atmospheric neutrinos

Hisakazu Minakata IFT UAM/CSIC, Madrid Chee Sheng Fong, HM, Hiroshi Nunokawa, arXiv:1609.08623, 1712.02798

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We see things converge

  • T2K see more and more preference of δ ~ 3π/2
  • T2K II (proposed, run unUl 2026) they could see

CPV at ~3 σ (expected for ~15x1021 POT)

  • δ ~ 3π/2 is the best case for NOvA for mass
  • rdering (see bi-P plot), will see mass hierarchy

at ~3 σ

  • Already Bari global analysis says “normal at 3 σ ”
  • Everybody vs NOvA discrepancy about θ23 seems

resolved best fit near maximal

  • We must think about what is next?

May 29, 2018 PANE@ICTP Trieste

My answer is “paradigm test”

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δ=3π/2 (or –π/2) implies that we are at the tip of the ellipse the best case for NOvA

May 29, 2018 PANE@ICTP Trieste

δ and sign Δm2

31 couple because

(Δm2

31 - Δm2 31 , δ π-δ)

symmetry in vacuum (JHEP 2001) Sign of Δm2

31 disUnguishes

normal vs inverted mass ordering P-\bar{P} bi-probability diagram, proposed by HM-H.Nunokawa, JHEP 2001

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SLIDE 4

May 29, 2018 PANE@ICTP Trieste

JUNO can measure |Ue1|2 +|Ue2|

2 +|Ue3|2

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JUNO can do Separate determinaUon |Ue1|2 and|Ue2|2 : 5 years

May 29, 2018 PANE@ICTP Trieste

1 – (|Ue1|2 +|Ue2|2 +|Ue3|2 ) can be constrained to ~1% level by JUNO !

Chee Sheng Fong, HM, Hiroshi Nunokawa, JHEP 2017

Resolve Δm2

31

  • vs. Δm2

32 waves

3% flux error assumed

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SLIDE 6

May 29, 2018 PANE@ICTP Trieste

High vs low scale unitarity violation

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New Physics at high energies:

  • This is Orthodox way, well studied ..
  • high scale UVpioneering work by Antusch,

Biggio, Fernandez-MarUnez, Gavela, and Lopez-Pavon, JHEP2006

  • But, neutrino experiments will not be the best

player for unitarity test

  • the reason is: high-energy SU(2) x U(1)

prevails charge lepton gives stronger constraints

May 29, 2018 PANE@ICTP Trieste

My suggesUon today is low-E UV

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SLIDE 8

New Physics at low energies: relaUvely new opUon

  • “low scale”: heavy leptons/neutrinos do

communicate with light ν system, i.e., parUcipate to nu oscillaUon

  • Various scenarios are proposed which involve

“new physics” at low energies: moUvated by LSND-MiniBoone, DAMA, etc.

  • Orthodoxy seems challenged, e.g., WIMP dark

maqer, low-E SUSY, day one NP, ..

May 29, 2018 PANE@ICTP Trieste

Plus many more !!

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High- vs low-energy unitarity violaUon

  • lepton flavor universality:

NO

  • zero distance neutrino

flavor transiUon: YES

  • KinemaUcal effect of

sterile nu emission: YES (if kinemaUcally allowed)

  • lepton flavor

universality: YES

  • zero distance neutrino

flavor transiUon: NO

  • KinemaUcal effect of

sterile nu emission: YES

May 29, 2018 PANE@ICTP Trieste

High-energy UV Low-energy UV

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SLIDE 10

May 29, 2018 PANE@ICTP Trieste

3 active+N- sterile ν model for Low-E unitarity violation

Other models of Low-E UV?

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3 acUve +N sterile unitary model in vacuum

May 29, 2018 PANE@ICTP Trieste

NxN 3x3

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3+N model for low-E UV and modest requests on it

  • By 3+N model I mean (3+N) space is unitary,

but not in 3 acUve nu space

  • Requirement: The predicUon of the 3+N

model must be independent of details of N sterile sector

  • Auer fulfilling this criterion we will show what

is the difference between High-E vs Low-E UV

May 29, 2018 PANE@ICTP Trieste

Unique? Probably not. General Low-E UV model hard to construct. My strategy is …

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Probability in vacuum

  • AcUve-acUve, acUve-sterile, sterile-sterile oscillaUons
  • If Δm2

as (Δm2 ss) > 0.1 eV2, “fast oscillaUon” due to

acUve-sterile and sterile-sterile Δm2 are averaged out

May 29, 2018 PANE@ICTP Trieste

What is this?

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P looks almost standard one, but there is a new term

May 29, 2018 PANE@ICTP Trieste

Appearance Disappearance

Probability leakage !

U = non-unitary “MNS” Order ~ W4, small!!

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P-leaking term: It must be obvious to exist, right?

  • There is a N sterile sector which can

communicate with acUve nu sector

  • So the probability leaks to sterile sector
  • Yet, not emphasized before…
  • ~ W4, Too small?

May 29, 2018 PANE@ICTP Trieste

Term kept by S. Parke and M. Ross Lonergan, PRD 2017 is also 4th order in W

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SLIDE 16

May 29, 2018 PANE@ICTP Trieste

Can one detect Cee? Invitation to non-unitary world..

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SensiUvity to Cee and 1-Σ|Uei|2 from JUNO 5 years

May 29, 2018 PANE@ICTP Trieste

Cee ~ 10-4 (1 σ) 1-Σ|Uei|2 ~ 0.01

3% flux uncertainty assumed

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Parke-Ross-Lonergan PRD2016

May 29, 2018 PANE@ICTP Trieste

Without P leaking term!

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Constraints on unitarity violaUon (Parke-Ross-Lonergan)

May 29, 2018 PANE@ICTP Trieste

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May 29, 2018 PANE@ICTP Trieste

Model- independent P: Prevail to “in matter” ?

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Small-UV perturbaUon theory

May 29, 2018 PANE@ICTP Trieste

Chee Sheng Fong, HM, Hiroshi Nunokawa, arXiv:1712.02798

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Small-UV perturbaUon theory: change to vacuum mass basis

May 29, 2018 PANE@ICTP Trieste

Do perturbaUon theory in hat basis X=unitary matrix, diagonalize H0(3x3)

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Do W perturbaUon to 4th order to keep P leaking term

  • Did we find ~W4 P leaking term? Yes!
  • How about what is the role of the rest?

May 29, 2018 PANE@ICTP Trieste

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May 29, 2018 PANE@ICTP Trieste

Typical W4 term

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May 29, 2018 PANE@ICTP Trieste

P leaking term

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Auer averaging out fast oscillaUons..

May 29, 2018 PANE@ICTP Trieste

Zeroth order in W 2nd order terms: Large denominator suppression Always comes with maqer potenUal

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A simple formula for oscillaUon probability in maqer w/o unitarity: leading order in W apart from Cαβ

  • All W2 & W4 terms avaraged out or suppressed if Δm2 > 0.1

eV2 except for P leaking term!!

  • UV effect is in: (1) explicit W correcUon term, (2) non-unitary

U matrix

May 29, 2018 PANE@ICTP Trieste

X=…

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May 29, 2018 PANE@ICTP Trieste

Where is the region

  • f large UV?
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SLIDE 29

May 29, 2018 PANE@ICTP Trieste

ΔP large at solar- and atm- MSW enhanced regions

  • Leading order

terms = Zeroth

  • rder in W
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May 29, 2018 PANE@ICTP Trieste

Large ~W2 corrections?

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  • Order W2 correcUon

terms

  • small in most
  • f the regions of L-E,

but sizeable in limited places

  • High energy, long

baseline IceCube, PINGU, Hyper-K

May 29, 2018 PANE@ICTP Trieste

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Conclusion (non-unitarity)

  • General structure of nu oscillaUon in acUve nu

sector of (3+N) unitary system is analyzed in vacuum and in maqer in the context of low-E unitarity violaUon

  • A new term, the “probability leaking term” found

(leaking to sterile sector)

  • DisUnguishes between Low-E vs High-E

unitarity violaUon

  • CondiUons for sterile sector model-independent P in

vacuum and in maqer are elucidated mJ

2 > 0.1 eV2

  • Likely to be insensiUve to sterile interacUons

May 29, 2018 PANE@ICTP Trieste

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SLIDE 33

Conclusion (non-unitarity2)

  • JUNO analysis shows one can constrain UV in νe

row at a high level

  • Cee ~ 10-4, 1-Σ|Uei|2 ~ 0.01 (both 1 σ)
  • Non-unitarity effect in the leading order (W0)

seems sizeable in solar- and atm MSW regions (Probability level)

  • generally requires L ~ 3000-104 km
  • W2 correcUon sizeable in limited L-E regions
  • disUnguishes between low-E from high-E UV
  • L ~ 3000-104 km

May 29, 2018 PANE@ICTP Trieste

Atmospheric nu important Atmospheric nu important