invading process of gcrs into the heliosphereheap18/slides/07_matsukiyo.pdfinvading process of gcrs...
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![Page 1: Invading process of GCRs into the heliosphereheap18/slides/07_Matsukiyo.pdfInvading process of GCRs into the heliosphere S. Matsukiyo1, K. Shimokawa1, H. Washimi1,2, T. Hada1 1Kyushu](https://reader034.vdocuments.site/reader034/viewer/2022050509/5f99ec8923f16f387a611bfe/html5/thumbnails/1.jpg)
Invading process of GCRs into the heliosphere
S. Matsukiyo1, K. Shimokawa1, H. Washimi1,2, T. Hada1
1Kyushu Univ., Japan2CSPAR, USA
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Background
Solar modulation of CR spectrum
Remarkable for E < a few 10 GeV
Anisotropy for TeV CRs
Effect of convected spiral SW B field
Effect of large scale structures (TS, HP)
Effect of wave-particle interactions
Effect of non-stationarity of SW
…Yuan [2018]
NASA
Abbasi et al. [2010]
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Background
Past approach
Diffusion-convection eq. based
Yuan (2018), Aloisio et al. (2015), Yamazaki et al. (2015),
…
Test particle simulation + global MHD simulation
Lopez-Barquero et al. (2016, 2017), …
∆ = 20 AU
3500 AU
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Purpose
To understand detailed process of GCR
invasion into the heliosphere and
further into the Earth
To reveal energy dependence of the
invasion process
Approach:
Test particle simulation + high resolution
global MHD simulation (∆ = 0.2 AU)
Washimi et al. [2015]
P T
V B
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Test particle simulation + MHD simulation
provided by Washimi
Test particle simulation using �, � fields
reproduced by MHD simulation
���
��� � �
�
�� � ,
���
��� �
# particles � 10�
No waves/turbulence
Initial distribution function
-- uniform on a sheet at a certain �
in interstellar space
-- monoenergetic jet along local � field
� � 10, �100 1000
�~ 10"�#, �100 "�# 1000"�#
$%&' � 3)"
#%&' � 23+,/.
/%&' � 0.1/cc
1%&' � 63003
$&4 � 35)"
#&4 � 400+,/.
/&4 � 5/��
1&4 � 1073
particles8
9:
at 1AU
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Field lines
Z=0 Y=0
L1: draping $%&' connected to spiral $&4
L2: spiral $&4
L3: draping $%&' B/BISM
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Field structure
Bow shock, heliopause, termination
shock are reproduced.
The above discontinuities and SW
current sheet form current layers.
BJ
9
:
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Particle behaviors (γ � 10)
Y Z Z
XX Y
Z=0 Y=0 X=0
Most of particles follow L3 field lines and pass outside the HP or are
mirror reflected at the HP
Some particles come in and out of the heliosphere when they come
close enough to the heliopause along the draping IS B field lines
A part of them reach the inner boundary (r = 50AU) of the polar region
Very few particles reach the inner boundary after a short time (weeks)
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Particle behaviors (γ � 10) Direction of field felt by a particle changes when it crosses the HP.
The particle stays near current sheet for a long time.
<� � 0.013
Dis
tan
ce f
rom
th
e s
un
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Particle behaviors (γ � 1000) Direction of field felt by a particle changes when it crosses the HP.
They do not stay in the current sheet due to large gyro radii.
<� � 1.3
Dis
tan
ce f
rom
th
e s
un
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Particle behaviors (γ � 1000) Easy to come in and out of the heliosphere due to large gyro radius
No mirror reflection for the particular case
Particles can reach the inner boundary (r = 50AU) with a short time
Some particles coil about the heliosphere even after that most of the
other particles flow away.
Y Z Z
XX Y
Z=0 Y=0 X=0
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Statistics Initial particle distribution:
uniform on a 1/8 sphere
velocity shell (uniform pitch angle)
# particles reached at inner boundary
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Statistics Energy dependence of anisotropy
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Summary
Test particle simulation of CR invasion process using EB field obtained by
global MHD simulation has been started.
Detailed analysis of particle behavior will be focused
Effect of wave-particle interaction will be incorporated
Statistics of particles will be discussed
…
Future Issues