motivation
DESCRIPTION
What is Role of Proton Beams in Solar Radio Bursts? Jun-ichi Sakai Laboratory for Plasma Astrophysics University of Toyama, Japan. Motivation. - PowerPoint PPT PresentationTRANSCRIPT
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What is Role of Proton Beams in Solar Radio
Bursts?
Jun-ichi Sakai Laboratory for Plasma Astrophysics
University of Toyama, Japan
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Motivation
• It is believed that solar radio bursts like Type III and Type II are generated from electrons accelerated in the solar flare region or from electrons accelerated near the fast magnetosonic shock front.
• It is recognized that some protons can be accelerated by surfing mechanism near the fast magnetosonic shock front. And also some protons are reflected and accelerated near the shock front, resulting in proton beams.
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Contents
• Proton acceleration by shocks--Surfing acceleration
• Examples of shock formation
• Wave emission from proton beams
• Conclusions
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Simulation Model
Solar surface
Magnetic Field Line
CME
Shock Wave
v
v
90°Model(1):90°
Model(2):90°
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Simulation Model
• Two-dimensional fully relativistic electromagnetic Particle-In-Cell code.
• System size: Lx=800, Ly=10
• The free boundary condition in the x-direction, and the periodic boundary condition in the y-direction are imposed.
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Initial Conditions and Parameters
0
x
y
E=v×B(Ez=vyBx)
B0v
10
200 8000
10
B=0n=4n0=400v=3vA=0.24c
B=B0
n=n0=100v=0
Mass ratio :mi=64me
Plasma beta :=0.05 (ce/pe=0.632) ce:Electron cyclotron frequencype:Electron plasma frequency
Alfvén velocity :vA=0.08c
(c=light velocity)
Model(1)
Model(2)
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Parameter Runs• Alfvén Mach (v/vA) : 3, 2, 1.5
• Propagation Angle () : 90°, 80°, 70°
(for Mach3)
90°, 70°, 40°
(for Mach2 and 1.5)
• Our simulation results are based on Alfvén Mach is 3 and Propagation Angle is 80°.
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Wave Emission Process
0.3
0.2
0.1
0.0
0.4
0.2
0.0
-0.2450400350300250
0.60.40.20.0-0.2
0.60.40.20.0-0.2
8006004002000
Ex
vex/c
vix/c
Ex
x
x
(pet=0)
(pet=90)
1.Some electrons are reflected behind the shock front.2.The reflected electrons behind the shock front mix up with the in-coming electrons due to the counter- streaming instability.3.Then there appear the electro- static waves behind the shock.
Shock region
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Particle Acceleration
-0.15-0.10
-0.05
0.00
0.05
-0.4
-0.2
0.0
0.2
0.4
450400350300250
3.0
2.0
1.0
0.08006004002000
3.0
2.0
1.0
0.0
ByBy
viz/c
vez/c
x
x (pet=0)
(pet=90)
Both electrons and ions arestrongly accelerated in the z-direction near the shock front
through the surfing mechanism.
Shock region
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Surfing Acceleration byElectrostatic wave propagating perpendicular to magnetic field
€
midv
dt= e(E +
v
c× B)
Equation of Motion Ex=E0sin(t-kx)By=B0
x
y
z
e
€
vz = −v phωcit + v0z
Acceleration Factor
Solve for vz
In moving frame
Ex
€
E⊥B
≈ ρ i (c
ω pe)−1 VA
2
cvth, i(MA − 1)3 / 2
Vmax
VA≈ (mime
)1/ 2 (MA − 1)3 / 2
ω ci tA ≈ MA−1ω piω ci
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Spatial Distribution of Ex and Ez Ex Ez
x x
(pet=18) (pet=66)0.03
0.02
0.01
0.00
-0.018006004002000
Red arrow area (x=70 〜 326) are used to find the dispersion relation of Ex.Blue arrow area (x=540 〜 796) are used to find the dispersion relation of Ez.
-0.04
-0.02
0.00
0.02
0.04
400300200100
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Dispersion Relations of Ex and Ez
-4 -2 0 2 4
4
3
2
1
2.5 3.0 3.5 4.0 4.5
-4 -2 0 2 4
4
3
2
1
0
0 1 2 3 4 5
/pe
kc/pe
/pe
kc/pe
Ex Ez
Elecrostatic Langmuir Waves (Z-mode) are generated in theyellow contour line.
EM Waves areexcited.
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• We found the wave emission process of Solar Type II Radio Bursts associated with CME.
• We also found that fast magnetic shock wave is formed with both protons and electrons accelerated by the surfing mechanism.
Conclusions
1. Some electrons are reflected behind the shock front. 2. Reflected electrons generate electrostatic waves. 3. They could be converted to the extra-ordinary electromagnetic waves through
the Direct Linear Mode Conversion.
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1.Generation of magnetosonic shocks during collision of two current loops
Simulation System
• PIC simulation
• Force-Free magnetic configuration– J×B = 0 – Uniform density and uniform
temperatur
• System size:– 900× 900– n0=100 – Loop position : (300, 300) & (600,
600)– Loop radius : 100 200 400 600 800
800
600
400
200
x
y
€
Bθ =B0r1 /a
1+ (r1 /a)2+
B0r2 /a
1+ (r2 /a)2
Bz =B0
1+ (r1 /a)2±
B0
1+ (r2 /a)2
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2.Generation of magnetosonic shock during formation of
current sheet
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Emission of electromagnetic waves by proton beams
The proton beams propagating to the low-density region are forced to move, together with the background electrons, to keep charge
neutrality, resulting in the excitation of electrostatic waves:
proton beam modes and Langmuir waves.
In the early stage of electrostatic wave excitation, both R and L modes near the fundamental plasma
frequency can be generated along a uniform magnetic field.
It is also found that, in the late stage, the second harmonics
of electromagnetic waves can be excited through the interaction of three waves. During these emission processes, proton
beams can move along the magnetic field almost without losing their kinetic energy.
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Electron(solid line) and Proton(dashed line) velocity distribution:
(a) t=0 and (b) pet=1500
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• Sakai and Nagasugi (2007) investigated the dynamics of proton beams propagating along a uniform magnetic field, as well as across the magnetic field in nonuniform solar plasmas, paying attention to the emission process of electromagnetic waves to understand a new solar-burst component emitting only in the terahertz range during the solar flare observed by Kaufmann et al.(2004).
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Proton beams propagating into high density region
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• From the simulation where the proton beams propagate along a uniform magnetic field into the high-density region, it is found that strong electromagnetic waves are generated behind the proton beams. When the proton beams propagate perpendicular to the magnetic field, the extra-ordinary mode can be excited from two electron Bernstein waves through three-wave interactions. These simulation results could be applied to the electromagnetic wave emission from the solar photosphere during the solar flares.
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Conclusions
1.Protons can be accelerated by surfing mechanism in shock front
2.Proton beams play an important role for the emission of electromagnetic waves
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• The role of proton beams reflected in the fast magnetosonic shock front is also discussed for the emission mechanism of the Type II radio bursts.
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Shock formation and double structure(60 degree)
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Time History of Ex and Ez
2x10-4
3
4
56
50454035302520
Ex Ez
pet pet
(Electrostatic) (Electromagnetic)
Parameters Red line: /pe=1.3 〜 1.6, kc/pe=0 〜 2.5Black line: /pe=1.5 〜 2.0, kc/pe=0 〜 3.0Blue line: /pe=2.5 〜 3.5, kc/pe=0 〜 4.0
Fundamental
Second harmonic
They are obtained by Inverse Fourier Transformationusing the data of dispersion relations.
54321
x10-5
7060504030