Calculation of Atmospheric Neutrino Flux Based on AMS02 Observation - - PowerPoint PPT Presentation

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Calculation of Atmospheric Neutrino Flux Based on AMS02 Observation - - PowerPoint PPT Presentation

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Calculation of Atmospheric Neutrino Flux Based on AMS02 Observation July 13, 2017 M. Honda @ ICRC2017 1. Cosmic Ray Observation of AMS02 and Some Others 2. Cosmic Spectra Model 3. Muon Calibration of Hadronic Interaction Model 4. Calculation

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SLIDE 1

Calculation of Atmospheric Neutrino Flux Based

  • n AMS02 Observation

July 13, 2017 M. Honda @ ICRC2017

  • 1. Cosmic Ray Observation of AMS02 and Some Others
  • 2. Cosmic Spectra Model
  • 3. Muon Calibration of Hadronic Interaction Model
  • 4. Calculation of Atmospheric Neutrino Flux
  • 5. Comparison with Previous Calculation and Estimation of Errors.
  • 6. Summary
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SLIDE 2

Primary Cosmic Ray Model and referred data (2004)

Other chemical compositions are also considered in the calculation, but they give small contributions.

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SLIDE 3

Balloon Borne (BESS) Satellite (ISS, AMS02)

Direct Observation

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SLIDE 4

Recent Cosmic Ray observation and Available High Energy data

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SLIDE 5

Proton Closeup

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SLIDE 6

Helium Closeup

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SLIDE 7

Cosmic Ray Spectra Model Based on AMS02 Observation

Looking forward to hearing from CALET and ISS-CREAM

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SLIDE 8

Solar Modulation and Neutron Monitor

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SLIDE 9

Solar Modulated Flux at Fixed Energy

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SLIDE 10

Practical Formula for Solar Modulation

Where a is from right figure, and N is the Count of Newark Neutron Monitor.

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SLIDE 11

Muon Calibration

Primary cosmic ray flux Interaction model Calculation scheme (include rigidity cutoff) Atmosphere model

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SLIDE 12

Muon Calibration of Interaction Model

Quick 3D Calculation for Muon flux. As the muon flux is a “local quantity” (γ ct 〜 60km at10 GeV ), We can calculate it in a quick calculation method:

  • 1. Inject cosmic rays just above the observation point,
  • 2. Analyze all muons reach the surface of Earth.
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SLIDE 13

Comparison of Quick 3D and Full 3D calculations

Full 3D Quick 3D

μ

+

μ

−

This method works above 0.2 GeV/c.

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SLIDE 14

Muon Calibration of inclusive DPMJET-III Data are larger by ~15% Data are larger by ~0.05 Data are smaller by ~0.05 ==> DPMJET-III Should be Modifjed ~15% scatter ?

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SLIDE 15

Comparison AFTER the modification

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SLIDE 16

JAM + Modified DPMJET-II vs Muons at the Balloon altitude ( HKKM2011) Good agreement ! Use DPMJET-III above 32 GeV and JAM below 32 GeV

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SLIDE 17
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SLIDE 18

With Cosmic ray spectra model based

  • n AMS02 observation

After muon re-calibration Before muon re-calibration

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SLIDE 19

Simulation Sphere (Rs = 10 x Re)

Full 3D-Calculation

Injection Sphere (Re +100lm)

Virtual Detector

The neutrino flux is calculated from the number of neutrinos path through with virtual detector correction.

Cosmic Rays are sampled and injected here

Re = 6378km

Cosmic ray go out this sphere are discarded. Cosmic rays go beyond are pass the rigidity cutofg test

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SLIDE 20

Atmosphere Model

Air density comparison with MSISE90 US-starndard'76 may be used as the global approximation of the Atmosphere.

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SLIDE 21

Kamioka INO site South Pole Near North Pole (Physalmi)

Atmosphere model (NRLMSISE-00) and seasonal variations

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SLIDE 22

IGRF10 Geomagnetic Horizontal Field Strength

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SLIDE 23

Based On AMS02 Obervation (Preliminary)

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SLIDE 24

Estimated Error in Atmospheric ν-flux Calculation (HKKMS07)   -observation error + Residual of reconstruction K  air

Kaon production uncertainty Mean free path (interaction crossection) uncertainty Atmosphere density profule uncertainty Possible Error with JAM (HKKM11)

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SLIDE 25

Summary

  • According to the new cosmic ray data provided by AMS02 and some
  • thers, We have renewed the Cosmic Ray Spectra Model including the

practical formula for the Solar Modulations.

  • The Muon Calibration of Hadronic Interaction Model was repeated

again, with the newly constructed Cosmic Ray Spectra Model.

  • The atmospheric neutrino flux calcuoated with New Cosmic Ray

Spectra Model and the Muon-Calibrated Hadronic Interaction Model wit it is generally similar to the previously calculated one, considering the difference of the Muon-Calibration Policy.

  • However, a ~ 5% deficit of the flux at ~ 10GeV is seen in the newly

calculated atmospheric neutrino flux irrespective of arriving directions

  • r kind of neutrinos.
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SLIDE 26

Comparison with Neutrino Data

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SLIDE 27

From K.Okumura in ICRC2015

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SLIDE 28

Best fit corresponds to 62 %

  • f the predicted variations

Solar Modulation of Atmospheric Neutrinos

From PHD thesis of

  • E. Richard

Poor Statistics

Picked up mainly the forbush decrease ?

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SLIDE 29

Observed Azimuthal Variation of flux (from PHD thesis of E.Richard)

νe

Zenith Angle Binned All Energies Energy Binned All Azimuth angles

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SLIDE 30

νμ

Observed Azimuthal Variation of flux (from PHD thesis of E.Richard)

Zenith Angle Binned All Energies Energy Binned All Azimuth angles

air

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SLIDE 31

Comparison in [Flux/depth]

DPMJET-III show the best agreement

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SLIDE 32

Pν=0.32

At GeV/c

π

± → νμ(̄

νμ)+ μ

±

p+ N(air)→ π

±+ X

μ

± → ̄

νμ(νμ)+ νe(̄ νe)+ e

±

Phase Space Study

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SLIDE 33

Pμ=0.32

At GeV/c

 pN air X

Size of Phase space to give the variation

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SLIDE 34

e  e   

Vertical neutrino flux

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SLIDE 35

e  e   

Horizontal neutrino flux

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Horizontal enhancement of neutrino fmux (Battistoni et al. Astropart. Phys 1999)

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SLIDE 37

Interpretation of horizontal enhancement Longer integration length in the neutrino production zone for horizontal directions