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Ionospheric electrodynamics and its coupling to the magnetosphere
Akimasa Yoshikawa
International Center for Space Weather Science and Education(ICSWSE)
Department of Earth and Planetary SciencesKyushu University, Japan
Outline (1) Fluid description (B,V) for partially ionized system
(2) M-I coupling via shear Alfven wave
・wave generation and propagation and their relation to velocity shear
・Plasma Equation of motions
・Generalized Ohm’s law
・atmospheric dynamo
・magnetospheric dynamo
・3D current closure inside ionosphere
Fundamental evolution equations of physical
quantities Qk
Qk = B,E,J,V,Vn
evolution of B-field
evolution of E-field∂∂tE =
∇×B( )− µ0 jε0µ0
∂∂tV = ?evolution of plasma velocity
evolution of current density∂∂tj = ?
evolution of neutral velocity∂∂tVn = ?
What’s drive What in the weakly ionized system?
momentum equations in the collisional system
mini∂∂tv i = eni E+ v i ×B( )−∇⋅ pi −miν inni v i − vn( )−meνeini v i − ve( )
for ion fluid
for electron fluid
for neutral fluid
(1)
(2)
(3)
Lorentz force kinetic tensormomentum exchangebetween plasma and
neutral
momentum exchange between electron and ion
ρn∂vn∂t
+ (vn .∇)vn⎡⎣⎢
⎤⎦⎥= −∇pn − ρnνni (vn −Vi )− ρnνne(vn −Ve )+ Fn
mene∂∂tve = −ene E+ ve ×B( )−∇⋅ pe −meνenne ve − vn( ) +meνeini v i − ve( )
momentum exchangeBetween ion and neutral
momentum exchangeBetween electron and
neutral
One fluid−description for global phenomena (Hall MHD approximation)
j = en v i − ve( ) V = miv i +mevemi +me
ρ = mi +me( )n
v i = V + me
ρe⎛⎝⎜
⎞⎠⎟j ve = V − mi
ρe⎛⎝⎜
⎞⎠⎟j
current density barycentric velocity mass density
ion velocity electron velocity
n = ni = neplasma density
P = Pi + Pepressure gradient
+ - << + - >> + - >> mi >> me
One-fluid description of ion and electron�(motion and current)
for ion minddtV + me
ρe⎛⎝⎜
⎞⎠⎟j
⎡
⎣⎢
⎤
⎦⎥ = en E+V ×Β( ) + me
mi +me
⎛⎝⎜
⎞⎠⎟j×B−minν in V − vn −
me
ρe⎛⎝⎜
⎞⎠⎟j
⎡
⎣⎢
⎤
⎦⎥ −
miν ie
e⎛⎝⎜
⎞⎠⎟ j−∇pi
for electron menddtV − mi
ρe⎛⎝⎜
⎞⎠⎟j
⎡
⎣⎢
⎤
⎦⎥ = −en E+V ×Β( ) + mi
mi +me
⎛⎝⎜
⎞⎠⎟j×B−menνen V − vn +
mi
ρe⎛⎝⎜
⎞⎠⎟j
⎡
⎣⎢
⎤
⎦⎥ −
meνei
e⎛⎝⎜
⎞⎠⎟ j−∇pe
current density (charge weighted form of velocity evolution)
equation of motion (mass weighted form of velocity evolution)
en ddtV + me
ρe⎛⎝⎜
⎞⎠⎟j
⎡
⎣⎢
⎤
⎦⎥ =
e2nmi
⎛⎝⎜
⎞⎠⎟E+V ×Β( ) + e me
mi
⎛⎝⎜
⎞⎠⎟j×Bmi +me
− enν in V − vn −me
ρe⎛⎝⎜
⎞⎠⎟j
⎡
⎣⎢
⎤
⎦⎥ −ν ie j−
e∇pimi
−en ddtV − mi
ρe⎛⎝⎜
⎞⎠⎟j
⎡
⎣⎢
⎤
⎦⎥ =
e2nme
⎛⎝⎜
⎞⎠⎟E+V ×Β( )− e mi
me
⎛⎝⎜
⎞⎠⎟j×Bmi +me
+ enνen V − vn +mi
ρe⎛⎝⎜
⎞⎠⎟j
⎡
⎣⎢
⎤
⎦⎥ +νei j+
e∇peme
ionic current
electron current
dominant partcancellation part
inertial part Lorentz force Ampere force momentum exchange to neutrals
momentum exchangebetween ion and electrons
ion : main portion of plasma dynamics electron : main portion of current carier
Generalized Equation of motion for one-fluid plasma
ρ ∂∂tV = j×B−∇P − n miν in +meνen( ) V −Vn( )−me ν in −νen( ) j
e
inertial
Ampere force
pressure gradient
momentum exchange between neutral andcharged particles
friction force along j
electromotive e-field
Hall e-field
am-bipolar field
emf
= V ×B+B ν in −νen( )
Ωe
V − vn( )− ∇pene
resistive e-field
convection electric field
electric field induced by momentum exchange effect
Generalized Ohm’s law
!R ⋅ j = B
ne⎛⎝⎜
⎞⎠⎟
νen +νei
Ωe
⎛⎝⎜
⎞⎠⎟j+ j× b( )⎡
⎣⎢
⎤
⎦⎥
∂∂tj = ε0ω pe
2 E+ emf! "!!
−#R ⋅ j( )
reactive-field
Distribution of collision frequency
controls the momentum exchange between neutral and charged particles
miν in > meνen
νen >>ν in
All altitudes
180km
νen >νei
80km
νen
Ωe
>1
ν in
Ωi
>1
140km
ν in >νei
110kmmax(νei )
νen
Ωe
<1ν in <νei
ν in
Ωi
<1νen <νei
From Song, et al., [2001]
Equation for motion of plasma (dominant)
inertial Ampere force pressure gradient forcemomentum exchange
between ion and neutralsfriction force along j
miν in >> meνen ν in <<νen
everywhere importantdominant
in the ionosphere important below 80kmimportant ω>~νin
Important near plasma sheet
∂∂tV = −ν in V −Vn( ) + j×B
ρ+ Bρ
νen
Ωe
⎛⎝⎜
⎞⎠⎟j− ∇P
ρ
Force balance Equation below �E-layer
inertial Ampere forcemomentum exchange between ion and neutrals
friction force along j
miν in >> meνen ν in <<νen
everywhere importantdominant
in the ionosphere important below 80km
0 ! −ν in V −Vn( ) + j×B
ρ+ Bρ
νen
Ωe
⎛⎝⎜
⎞⎠⎟j
ω <<ν inWith cold plasma plasma approximation
Ionospheric current is� a force balance current
j×B = en ken2
1+ ken2
⎛⎝⎜
⎞⎠⎟kin−1 V −Vn( ) + ken
1+ ken2
⎛⎝⎜
⎞⎠⎟kin−1 V −Vn( )×B⎧
⎨⎩⎪
⎫⎬⎭⎪
j×B ! kin−1en V −Vn( )
For 90km~140km Important only for 80km Atmospheric dynamo through collision via electron
(dynamo region-> 70~90km)
Atmospheric dynamo through collision via ion(dynamo region-> 90~140km)
kin ≡
ν inΩi
⎛
⎝⎜⎞
⎠⎟ ken ≡
νenΩe
⎛
⎝⎜⎞
⎠⎟
plasma – neutral interaction j×B ≅ ρν in V − un( )
j×B( ) ⋅V" ≅ ρν in V" 2 V ' ≅ V − un
In the neutral frame
j×B( ) ⋅v ≅ ρν in V − un( ) ⋅v = j ⋅E
j ⋅E > 0 for v > un j ⋅E < 0 for v < un
Work done by Ampere force = work done by momentum exchange by collision
Atmospheric load Atmospheric dynamo
Electromagnetic energy is converted into mechanical energy
Electromagnetic energy is generated from mechanical energy
Equivalence of electromagnetic load and mechanical load
Work done by Ampere force = heating by plasma
In the rest (plasma) frame
Atmospheric dynamo
neutral wind
Plasma flow (within the dynamo region)
Magnetic perturbation, current
Electric field (within the dynamo region)
Momentum exchange by Ion-neutral collision
Generalized Ohm”s law
Non-zero curl E (different E within and outside dynamo region along B0)
Plasma flow out side dynamo region Ampre froce (magnetic tension acting plasma )
To the magnetosphere Alfven wave generation
Atomospheric dynamo j×B( ) ⋅V ! kin−1en V −Vn( ) ⋅V
Work done by Ampere force acting on ion Work done by momentum exchange between ion and neutral on ion
j×B( ) ⋅V ! kin−1en V −Vn( ) ⋅V > 0Case (A) if
Ampere force can accelerate neutrals through collision(atmospheric load)
j×B( ) ⋅V ! kin−1en V −Vn( ) ⋅V < 0Neutral particle can produces Ampere force through
Collision (electromagnetic energy is produced by kinetic energy of Neutral particles) (atmospheric dynamo)
Case (B) if
Generalized Ohm’s law (dominant)
Electromotive e.m.f. e-field
∂∂tj = ε0ω pe
2 E+ emf! "!!
−#R ⋅ j( )
Hall e-fieldresistive e-field
convection e- field e-field induced by
momentum exchange between electron and neutral
!R ⋅ j = B
ne⎛⎝⎜
⎞⎠⎟
νen
Ωe
⎛⎝⎜
⎞⎠⎟j⊥ + j× b( )⎡
⎣⎢
⎤
⎦⎥
Current evolution equation
e-field
reactive-field
emf! "!!
= V ×B− B νen
Ωe
⎛⎝⎜
⎞⎠⎟V − vn( )
Electromagnetic wave Radiationevolution of B-field evolution of E-field
∂∂tE =
∇×B( )− µ0 jε0µ0
1c2
∂2
∂t 2E+∇× ∇×E( ) = −µ0
∂∂tj evolution eq of J?
no!! electromagnetic field radiations eq by changing of current(like a dipole antenna)
we need to know how J is produced by electro-dynamics (not -magnetics)
∂∂tj = ε0ω pe
2 E− emf
−Rj( )
Rj = B
ne⎡⎣⎢
⎤⎦⎥
νen +νei
Ωe
⎛⎝⎜
⎞⎠⎟j+ j× b
⎡
⎣⎢
⎤
⎦⎥
Ohm’s law in ion-collisional system
j×B ! kin−1en V −Vn( )
emf! "!!# −V ×B
E = −V ×B+ kin−1B V − vn( )
!R ⋅ j " B
ne⎛⎝⎜
⎞⎠⎟ j× b( )
= kin−1B v i − vn( )
Eq of motion (force balance) Generalized Ohm’s law
Convection e-field
E+ vn ×B = − V − vn( )×B+ kin−1B V − vn( )
E* = −V* ×B+ kin−1BV*
Hall e-field
Ion-collisional resistive e-field
Ohm’s law in the neutral frame
E = emf! "!!
+#R ⋅ j
Ohm’s law in the rest frame
In the ionosphere electric field is induced not only in–VxB (convection electric field) direction but also
in the direction of plasma flow !!(very different from magnetosphere)
E* = E+ vn ×BV* = V − vn
E = emf! "!!
+#R ⋅ j
Magnetospheric Generator
“Generator” region can be defined as a region enable to production of velocity shear (vorticity) both parallel and perpendicular direction to B0 by the mechanical balance.
∇× v( )// ∝ ∇⋅E⊥( ) eB
v⊥ = E× eBB0
Parallel shear induces (div E⊥)
perpendicular shear produces (rot E⊥) .∂∂sv⊥ ∝ ∇× v( )⊥ ∝ ∇×E⊥( )⊥
∇× v( )// ∇× v( )⊥
Note: ∇⋅ ∇ × v( ) = 0 ∇ // ⋅ ∇ × v( )// = −∇⊥ ⋅ ∇ × v( )⊥Vorticity conservation as like a current
B0
∇⋅ j = 0 ∇ // ⋅ j// = −∇⊥ ⋅ j⊥
j⊥ = B0ΣA ∇× v( )⊥
j// = B0ΣA ∇× v( )//
∇⋅ j⊥ = 0 ∇⋅ ∇ × v( ) = 0
Shear Alfven wave
Always inductive!!
Induction process: generation and propagation shear Alfven wave
(1) Generator :drives enhanced convection velocity by balance of acceleration by pressure gradient force and deceleration by the magnetic tension force
(2) velocity shear along corresponds to rot(E) → development of magnetic field
→ development of tension force→ acceleration of
plasma flow at wave front
・ role of shear Alfven wave → disappearance of velocity shear along B0
・ Generator acts until difference of convection velocity along B0 is disappeared
∂∂sV⊥ ∝ ∇×E( )⊥ ∝ ∂
∂tb⊥ → j×B0 → ρ ∂
∂tV⊥
V0
V
Generator
E0
B0
j×B0( ) ⋅v0 > 0 −∇p ⋅v0 < 0
∇ // ⋅S// > 0
VAAlfven Induction loop responsible for A.Y
Magnetospheric dynamo
Magnetic perturbation, current
Electric field (within the dynamo region)
Generalized Ohm”s law
Non-zero curl E (different E within and outside dynamo region along B0)
Plasma flow out side dynamo region Ampre froce (magnetic tension force acting plasma )
Enhanced convection velocity (plasma flow within the dynamo region)
Alfven induction loop
velocity shear along corresponds to rot(E) → development of magnetic field
→ development of tension force→ acceleration of
plasma flow at wave front
To the ionosphere
Propagation of electromagnetic field inside the ionosphere�and production of reflection field
Ampere force
Ion collision Alfven-induction loop
velocity shear along B0 corresponds to rot(E)⊥ → development of magnetic field → development of tension force → acceleration of ion flow → braking of ion flow by collision
attenuation of vi No attenuation of ve
→ no braking of electron flow
Motion of ion induces two types electric field(1) Convection electric field
(2) Hall electric field Attenuation of vi through collisionCorresponds to attenuation of type (1) e-field
Equivalent to generation of oppositelydirected e-field
Magnetic perturbation, current
Shear (rot) of e-field along B-field
Generalized Ohm’s law
Plasma flow out side dynamo region
To the magnetosphere
(1) reflection Alfven-induction loop
From the magnetosphere
Process (1)
Propagation of electromagnetic field inside the ionosphere�and production of reflection field
Ampere force
Ion collision Alfven-induction loop
velocity shear along B0 corresponds to rot(E)⊥ → development of magnetic field → development of tension force → acceleration of ion flow → braking of ion flow by collision
attenuation of vi No attenuation of ve
→ no braking of electron flow
Generation of e-field in the direction vi
Shear of e-field along B0
Magnetic perturbation, current
This e-filed perpendicular to convection type e-field
Generalized Ohm’s law
Plasma flow out side dynamo region
To the magnetosphere
Hall dynamo Alfven-induction loop
From the magnetosphere
Motion of ion induces two types electric field(1) Convection electric field
(2) Hall electric field Process (2)