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Study of the Solar Magnetic Field influence on the cosmic ray Sun shadow
Nan Yuncheng Shandong University & Institute of High Energy Physics
Chen Songzhan, Feng Cunfeng and Jiang Chaowei
36th ICRC, 2019, Madison, WI, U.S.A
IHEP
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Outline
1. Introduction
2. Sun Shadow Modeling and the Solar-terrestrial Magnetic Field affection
3. Influences of Different CMF’s Models on the Sun Shadow
4. Summary
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Sun
1. Introduction
A probe to detect the Solar-terrestrial magnetic field.
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Sun shadow
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Interplanetary Magnetic Field: ARGO-YBJ probes the IMF using Sun shadow at 5 TeV.
ApJ, 729:113 (2011)
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The structure of the IMF estimated using Sun shadow
is consistent with the satellite measurement.
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The CSSS model is more consistent with the Sun shadow measurement.
Coronal Magnetic Field: Tibet ASγ evaluates two models using Sun shadow at 10 TeV.
PRL,111,011101(2013)
CSSS model is preferred.
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Energy dependent:ARGO-YBJ’s Result
ARGO-YBJ have detected Yearly rigidity dependence of Sun shadow. Chen, et al. 35th ICRC
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LHAASO’s expectation of 2-day Sun shadow observations
Wu, et al. Astroparticle Physics 103 (2018) 41–48
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2. SUN SHADOW MODELING AND THE SOLAR-TERRESTRIAL MAGNETIC FIELD AFFECTION
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Simulation of the Sun Shadow
• Back forward method
tracing the anti-particle from earth to Sun.
Earth
Sun
Anti-particle
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• Component: proton
• Energy range:TeV - PeV
• Number of events:~ 107
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The Solar-terrestrial Magnetic Field
IGRF model Rearth [T] Parker model θ =90°[nT] PFSS model[Gauss]
Large-scale magnetic field in the corona (CMF)
Interplanetary magnetic field (IMF)
Geomagnetic field
(GMF)
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Influence of Large-scale CMF on the Sun Shadow
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The CMF dominates the deficit ratio of the Sun shadow!
E=1TeV
West East(deg)
Sou
th
No
rth
(deg
)
E=10TeV
West East(deg)
Sou
th
No
rth
(deg
)
E=100TeV
Sou
th
No
rth
(deg
)
West East(deg)
Solar minimum
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Influence of Large-scale CMF on the Sun Shadow
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How?
E=1TeV
E=10TeV
E=100TeV
X(R⊙ )
Z(R⊙
)
X(R⊙ )
Z(R⊙
)
X(R⊙ )
Z(R⊙
)
SUN
SS Solar minimum
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Influence of IMF on the Sun Shadow
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Spring Equinox Summer Solstice Autumnal Equinox
we expect the seasonal dependence of the extension of the Sun shadow.
Seasonal dependence
A year
Solar minimum
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3. INFLUENCES OF DIFFERENT CMF’S MODELS ON THE SUN SHADOW
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Influences of Different CMF’s Models on the Sun Shadow
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Solar minimum
E< 10TeV, the CSSS and low height of Rss of the PFSS increase the extension!
At 10TeV, the deficit ratios of different models are the same! Different results from ASγ.
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Influences of Different CMF’s Models on the Sun Shadow
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Solar maximum
To explore more about the CMF, we need the experimental data and more simulation!
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• The CMF and the IMF affect the deficit and the extension of the Sun shadow, respectively.
• From our simulation, we expect the seasonal dependence of the extension of the Sun shadow.
• Also, current models and parameters give a different expectations on Sun shadow. Both of them need data to confirm.
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THANK YOU!
4. Summary