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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
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
Sun
1. Introduction
A probe to detect the Solar-terrestrial magnetic field.
-1-
Sun shadow
Interplanetary Magnetic Field: ARGO-YBJ probes the IMF using Sun shadow at 5 TeV.
ApJ, 729:113 (2011)
-2-
The structure of the IMF estimated using Sun shadow
is consistent with the satellite measurement.
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.
-3-
Energy dependent:ARGO-YBJ’s Result
ARGO-YBJ have detected Yearly rigidity dependence of Sun shadow. Chen, et al. 35th ICRC
-4-
LHAASO’s expectation of 2-day Sun shadow observations
Wu, et al. Astroparticle Physics 103 (2018) 41–48
-5-
2. SUN SHADOW MODELING AND THE SOLAR-TERRESTRIAL MAGNETIC FIELD AFFECTION
Simulation of the Sun Shadow
• Back forward method
tracing the anti-particle from earth to Sun.
Earth
Sun
Anti-particle
-6-
• Component: proton
• Energy range:TeV - PeV
• Number of events:~ 107
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)
-7-
Influence of Large-scale CMF on the Sun Shadow
-8-
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
Influence of Large-scale CMF on the Sun Shadow
-9-
How?
E=1TeV
E=10TeV
E=100TeV
X(R⊙ )
Z(R⊙
)
X(R⊙ )
Z(R⊙
)
X(R⊙ )
Z(R⊙
)
SUN
SS Solar minimum
Influence of IMF on the Sun Shadow
-10-
Spring Equinox Summer Solstice Autumnal Equinox
we expect the seasonal dependence of the extension of the Sun shadow.
Seasonal dependence
A year
Solar minimum
3. INFLUENCES OF DIFFERENT CMF’S MODELS ON THE SUN SHADOW
Influences of Different CMF’s Models on the Sun Shadow
-11-
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.
Influences of Different CMF’s Models on the Sun Shadow
-12-
Solar maximum
To explore more about the CMF, we need the experimental data and more simulation!
• 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.
-13-
THANK YOU!
4. Summary