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Transcript of Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.
![Page 1: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/1.jpg)
Basic Plasma Physics Principles
Gordon EmslieOklahoma State University
![Page 2: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/2.jpg)
Outline
Single particle orbits; drifts
Magnetic mirroring
MHD Equations
Force-free fields
Resistive Diffusion
The Vlasov equation; plasma waves
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Single particle orbits - drifts
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Single particle orbits
E and B fields are prescribed; particles are “test particles”
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Single particle orbits
F = q (E + v B)
Set E = 0 (for now)
F = q v B
Since F v, no energy gain (F.v = 0)
Particles orbit field line
mv2/r = qvB
r = mv/qB (gyroradius)
= v/r = qB/m (gyrofrequency)
![Page 6: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/6.jpg)
Single particle orbits
F = q (E + v B)
Set E = 0 (for now)
F = q v B
Since F v, no energy gain (F.v = 0)
Particles orbit field line
mv2/r = qvB
r = mv/qB (gyroradius)
= v/r = qB/m (gyrofrequency)
![Page 7: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/7.jpg)
Single particle orbits
F = q (E + v B)
Set E = 0 (for now)
F = q v B
Since F v, no energy gain (F.v = 0)
Particles orbit field line
mv2/r = qvB
r = mv/qB (gyroradius)
= v/r = qB/m (gyrofrequency)
![Page 8: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/8.jpg)
Single particle orbits
F = q (E + v B)
Set E = 0 (for now)
F = q v B
Since F v, no energy gain (F.v = 0)
Particles orbit field line
mv2/r = qvB
r = mv/qB (gyroradius)
= v/r = qB/m (gyrofrequency)
![Page 9: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/9.jpg)
Single particle orbits
F = q (E + v B)
Set E = 0 (for now)
F = q v B
Since F v, no energy gain (F.v = 0)
Particles orbit field line
mv2/r = qvB
r = mv/qB (gyroradius)
= v/r = qB/m (gyrofrequency)
![Page 10: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/10.jpg)
Motion in a Uniform Magnetic Field
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Motion in a Uniform Magnetic Field
Is this an electron or an ion?
![Page 12: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/12.jpg)
Motion in a Uniform Magnetic Field
Is this an electron or an ion?
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DriftsF = q (E + v B)
Now let E 0.
Relativistic transformation of E and B fields:
E' = γ(E + (v/c) B)
B' = γ(B – (v/c) E)
E'2 – B'2 = E2 – B2
If E < B (so that E2 – B2 < 0), transform to frame in which E = 0:
v = c (E B)/B2
In this frame, we get simple gyromotion
So, in ‘lab’ frame, we get gyro motion, plus a drift, at speed
vD = c (E B)/B2
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DriftsF = q (E + v B)
Now let E 0.
Relativistic transformation of E and B fields:
E' = γ(E + (v/c) B)
B' = γ(B – (v/c) E)
E'2 – B'2 = E2 – B2
If E < B (so that E2 – B2 < 0), transform to frame in which E = 0:
v = c (E B)/B2
In this frame, we get simple gyromotion
So, in ‘lab’ frame, we get gyro motion, plus a drift, at speed
vD = c (E B)/B2
![Page 15: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/15.jpg)
DriftsF = q (E + v B)
Now let E 0.
Relativistic transformation of E and B fields:
E' = γ(E + (v/c) B)
B' = γ(B – (v/c) E)
E'2 – B'2 = E2 – B2
If E < B (so that E2 – B2 < 0), transform to frame in which E = 0:
v = c (E B)/B2
In this frame, we get simple gyromotion
So, in ‘lab’ frame, we get gyro motion, plus a drift, at speed
vD = c (E B)/B2
![Page 16: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/16.jpg)
DriftsF = q (E + v B)
Now let E 0.
Relativistic transformation of E and B fields:
E' = γ(E + (v/c) B)
B' = γ(B – (v/c) E)
E'2 – B'2 = E2 – B2
If E < B (so that E2 – B2 < 0), transform to frame in which E = 0:
v = c (E B)/B2
In this frame, we get simple gyromotion
So, in ‘lab’ frame, we get gyro motion, plus a drift, at speed
vD = c (E B)/B2
![Page 17: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/17.jpg)
E B drift
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Drifts
Exercise:
What if E > B?
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DriftsvD = c (E B)/B2
E is “equivalent electric field”
Examples:
(1) E is actual electric field: vD = c (E B)/ B2 (independent of sign of q)
(2) Pressure gradient: qE = -p: vD = -cp B/qB2 (dependent on sign of q)
(3) Gravitational field: mg = qE: vD = (mc/q) g B/B2 (dependent on m and sign of q)
Puzzle: in absence of magnetic field, particles subject to g accelerate at the same rate and in the same direction; particles subject to E accelerate in opposite directions at a rate which depends on their mass. Why is the exact opposite true when a B is present?
![Page 20: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/20.jpg)
DriftsvD = c (E B)/B2
E is “equivalent electric field”
Examples:
(1) E is actual electric field: vD = c (E B)/ B2 (independent of sign of q)
(2) Pressure gradient: qE = -p: vD = -cp B/qB2 (dependent on sign of q)
(3) Gravitational field: mg = qE: vD = (mc/q) g B/B2 (dependent on m and sign of q)
Puzzle: in absence of magnetic field, particles subject to g accelerate at the same rate and in the same direction; particles subject to E accelerate in opposite directions at a rate which depends on their mass. Why is the exact opposite true when a B is present?
![Page 21: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/21.jpg)
DriftsvD = c (E B)/B2
E is “equivalent electric field”
Examples:
(1) E is actual electric field: vD = c (E B)/ B2 (independent of sign of q)
(2) Pressure gradient: qE = -p: vD = -cp B/qB2 (dependent on sign of q)
(3) Gravitational field: mg = qE: vD = (mc/q) g B/B2 (dependent on m and sign of q)
Puzzle: in absence of magnetic field, particles subject to g accelerate at the same rate and in the same direction; particles subject to E accelerate in opposite directions at a rate which depends on their mass. Why is the exact opposite true when a B is present?
![Page 22: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/22.jpg)
DriftsvD = c (E B)/B2
E is “equivalent electric field”
Examples:
(1) E is actual electric field: vD = c (E B)/ B2 (independent of sign of q)
(2) Pressure gradient: qE = -p: vD = -cp B/qB2 (dependent on sign of q)
(3) Gravitational field: mg = qE: vD = (mc/q) g B/B2 (dependent on m and sign of q)
Puzzle: in absence of magnetic field, particles subject to g accelerate at the same rate and in the same direction; particles subject to E accelerate in opposite directions at a rate which depends on their mass. Why is the exact opposite true when a B is present?
![Page 23: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/23.jpg)
DriftsvD = c (E B)/B2
E is “equivalent electric field”
Examples:
(1) E is actual electric field: vD = c (E B)/ B2 (independent of sign of q)
(2) Pressure gradient: qE = -p: vD = -cp B/qB2 (dependent on sign of q)
(3) Gravitational field: mg = qE: vD = (mc/q) g B/B2 (dependent on m and sign of q)
Puzzle: in absence of magnetic field, particles subject to g accelerate at the same rate and in the same direction; particles subject to E accelerate in opposite directions at a rate which depends on their mass. Why is the exact opposite true when a B is present?
![Page 24: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/24.jpg)
Magnetic Mirroring
Adiabatic invariants
Slow change of ambient parameters: Action p dq (e.g. Energy/frequency) is conserved
Apply this to gyromotion: E = (1/2) mv2; Ω = eB/m
Then as B slowly changes, mv2/(B/m) = m2v
2/B = p2/B is
conserved
As B increases, p increases and so, to conserve energy, p must decrease. This can be expressed as a mirror force
F = - (p2/2m) (B/B),
This force causes particles to be trapped in loops with high field strengths at the ends. Note that a magnetic compression also acts as a reflecting wall; this will help us understand particle acceleration later.
![Page 25: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/25.jpg)
Magnetic Mirroring
Adiabatic invariants
Slow change of ambient parameters: Action p dq (e.g. Energy/frequency) is conserved
Apply this to gyromotion: E = (1/2) mv2; Ω = eB/m
Then as B slowly changes, mv2/(B/m) = m2v
2/B = p2/B is
conserved
As B increases, p increases and so, to conserve energy, p must decrease. This can be expressed as a mirror force
F = - (p2/2m) (B/B),
This force causes particles to be trapped in loops with high field strengths at the ends. Note that a magnetic compression also acts as a reflecting wall; this will help us understand particle acceleration later.
![Page 26: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/26.jpg)
Magnetic Mirroring
Adiabatic invariants
Slow change of ambient parameters: Action p dq (e.g. Energy/frequency) is conserved
Apply this to gyromotion: E = (1/2) mv2; Ω = eB/m
Then as B slowly changes, mv2/(B/m) = m2v
2/B = p2/B is
conserved
As B increases, p increases and so, to conserve energy, p must decrease. This can be expressed as a mirror force
F = - (p2/2m) (B/B),
This force causes particles to be trapped in loops with high field strengths at the ends. Note that a magnetic compression also acts as a reflecting wall; this will help us understand particle acceleration later.
![Page 27: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/27.jpg)
Magnetic Mirroring
Adiabatic invariants
Slow change of ambient parameters: Action p dq (e.g. Energy/frequency) is conserved
Apply this to gyromotion: E = (1/2) mv2; Ω = eB/m
Then as B slowly changes, mv2/(B/m) = m2v
2/B = p2/B is
conserved
As B increases, p increases and so, to conserve energy, p must decrease. This can be expressed as a mirror force
F = - (p2/2m) (B/B),
This force causes particles to be trapped in loops with high field strengths at the ends. Note that a magnetic compression also acts as a reflecting wall; this will help us understand particle acceleration later.
![Page 28: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/28.jpg)
Plasma physics in principle
• Solve equations of motion with initial E and B:
md2ri/dt2 = qi (E + [dri/dt] B)• Then use the resulting ri and dri/dt to get charge
density ρ(r) and current density j(r)• Then obtain the self-consistent E and B through
Maxwell’s equations:.E = ρ
B = (4/c)(j + E/t)• “Lather, rinse, repeat”
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Plasma physics in principle
• Solve equations of motion with initial E and B:
md2ri/dt2 = qi (E + [dri/dt] B)• Then use the resulting ri and dri/dt to get charge
density ρ(r) and current density j(r)• Then obtain the self-consistent E and B through
Maxwell’s equations:.E = ρ
B = (4/c)(j + E/t)• “Lather, rinse, repeat”
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Plasma physics in principle
• Requires the solution of ~ 1027 coupled equations of motion
• Not a practical method!
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MHD Equations
• Replace ~ 1027 coupled equations of motion by “averaged” fluid equations
• Neglect displacement current (plasma responds very quickly to charge separation); then body force
F = (1/c) j B = (1/4) (B) B
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Complete set of MHD Equations
Continuity: /t + .(v) = 0
Momentum: dv/dt = -p + (1/4) (B) B - g
Energy: ?? (can use polytrope: d(p/γ)/dt = 0)
Induction: B/t = (v B)
These are 4 equations for the 4 unknowns
(, p, v, B)
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Force – Free FieldsEquation of motion is
dv/dt = - p + (1/4) (B)BDefine the plasma β = ratio of terms on RHS = p/(B2/8)For typical solar corona,
p = 2nkT ~ 2(1010)(1.38 10-16)(107) ~ 10B ~ 100
β ~ 10-3
So second term on RHS dominates, and in steady-state j must be very nearly parallel to B, i.e.
(B)B 0
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Force – Free FieldsEquation of motion is
dv/dt = - p + (1/4) (B)BDefine the plasma β = ratio of terms on RHS = p/(B2/8)For typical solar corona,
p = 2nkT ~ 2(1010)(1.38 10-16)(107) ~ 10B ~ 100
β ~ 10-3
So second term on RHS dominates, and in steady-state j must be very nearly parallel to B, i.e.
(B)B 0
![Page 35: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/35.jpg)
Force – Free FieldsEquation of motion is
dv/dt = - p + (1/4) (B)BDefine the plasma β = ratio of terms on RHS = p/(B2/8)For typical solar corona,
p = 2nkT ~ 2(1010)(1.38 10-16)(107) ~ 10B ~ 100
β ~ 10-3
So second term on RHS dominates, and in steady-state j must be very nearly parallel to B, i.e.
(B)B 0
![Page 36: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/36.jpg)
Force – Free Fields(B)B = 0
Solutions:(1) B = 0 (trivial)(2) B = 0 (current-free – “potential” field)(3) Linear case: (B) = αB(4) Full case: (B) = α(r)B
Note that taking the divergence of (B) = α(r)B
gives 0 = α.B + α .B, so that B.α = 0, i.e., α is constant on a field line.
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Force – Free Fields(B)B = 0
Solutions:(1) B = 0 (trivial)(2) B = 0 (current-free – “potential” field)(3) Linear case: (B) = αB(4) Full case: (B) = α(r)B
Note that taking the divergence of (B) = α(r)B
gives 0 = α.B + α .B, so that B.α = 0, i.e., α is constant on a field line.
![Page 38: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/38.jpg)
Force – Free Fields(B)B = 0
Solutions:(1) B = 0 (trivial)(2) B = 0 (current-free – “potential” field)(3) Linear case: (B) = αB(4) Full case: (B) = α(r)B
Note that taking the divergence of (B) = α(r)B
gives 0 = α.B + α .B, so that B.α = 0, i.e., α is constant on a field line.
![Page 39: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/39.jpg)
Force – Free Fields(B)B = 0
Solutions:(1) B = 0 (trivial)(2) B = 0 (current-free – “potential” field)(3) Linear case: (B) = αB(4) Full case: (B) = α(r)B
Note that taking the divergence of (B) = α(r)B
gives 0 = α.B + α .B, so that B.α = 0, i.e., α is constant on a field line.
![Page 40: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/40.jpg)
Force – Free Fields(B)B = 0
Solutions:(1) B = 0 (trivial)(2) B = 0 (current-free – “potential” field)(3) Linear case: (B) = αB(4) Full case: (B) = α(r)B
Note that taking the divergence of (B) = α(r)B
gives 0 = α.B + α .B, so that B.α = 0, i.e., α is constant on a field line.
![Page 41: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/41.jpg)
Force – Free Fields(B)B = 0
Solutions:(1) B = 0 (trivial)(2) B = 0 (current-free – “potential” field)(3) Linear case: (B) = αB(4) Full case: (B) = α(r)B
Note that taking the divergence of (B) = α(r)B
gives 0 = α.B + α .B, so that B.α = 0, i.e., α is constant on a field line.
![Page 42: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/42.jpg)
Resistive DiffusionConsider the Maxwell equation
E = - (1/c) B/t,together with Ohm’s law
Elocal = E + (v/c) B = ηj = (ηc/4) BCombined, these give:
B/t = (v B) - (ηc2/4) (B),i.e.
B/t = (v B) + D 2B,where D = ηc2/4 is the resistive diffusion coefficient.
![Page 43: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/43.jpg)
Resistive DiffusionConsider the Maxwell equation
E = - (1/c) B/t,together with Ohm’s law
Elocal = E + (v/c) B = ηj = (ηc/4) BCombined, these give:
B/t = (v B) - (ηc2/4) (B),i.e.
B/t = (v B) + D 2B,where D = ηc2/4 is the resistive diffusion coefficient.
![Page 44: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/44.jpg)
Resistive DiffusionConsider the Maxwell equation
E = - (1/c) B/t,together with Ohm’s law
Elocal = E + (v/c) B = ηj = (ηc/4) BCombined, these give:
B/t = (v B) - (ηc2/4) (B),i.e.
B/t = (v B) + D 2B,where D = ηc2/4 is the resistive diffusion coefficient.
![Page 45: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/45.jpg)
Resistive DiffusionB/t = (v B) + D 2B
The magnetic flux through a given contour S is given by
= S B. dS.The change in this flux is given by
d/dt = S B/t - E. d,where the second term is due to Faraday’s law. If
the electric field is generated due to cross-field fluid motions, then, using Stokes’ theorem
E. d = S E. dS = S (v B). dS we see that
d/dt = S [B/t - (v B)] dS = S D 2B dS.
Thus, if D=0, the field is frozen in to the plasma; the flux through an area stays constant as the area deforms due to fluid motions. If, on the other hand, D 0, then the flux can change (and as a result the energy in the magnetic field can be released).
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Resistive DiffusionB/t = (v B) + D 2B
The magnetic flux through a given contour S is given by
= S B. dS.The change in this flux is given by
d/dt = S B/t - E. d,where the second term is due to Faraday’s law. If
the electric field is generated due to cross-field fluid motions, then, using Stokes’ theorem
E. d = S E. dS = S (v B). dS we see that
d/dt = S [B/t - (v B)] dS = S D 2B dS.
Thus, if D=0, the field is frozen in to the plasma; the flux through an area stays constant as the area deforms due to fluid motions. If, on the other hand, D 0, then the flux can change (and as a result the energy in the magnetic field can be released).
B
dS
Φ
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Resistive DiffusionB/t = (v B) + D 2B
The magnetic flux through a given contour S is given by
= S B. dS.The change in this flux is given by
d/dt = S B/t - E. d,where the second term is due to Faraday’s law. If
the electric field is generated due to cross-field fluid motions, then, using Stokes’ theorem
E. d = S E. dS = S (v B). dS we see that
d/dt = S [B/t - (v B)] dS = S D 2B dS.
Thus, if D=0, the field is frozen in to the plasma; the flux through an area stays constant as the area deforms due to fluid motions. If, on the other hand, D 0, then the flux can change (and as a result the energy in the magnetic field can be released).
dΓE
B
dS
Φ
![Page 48: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/48.jpg)
Resistive DiffusionB/t = (v B) + D 2B
The magnetic flux through a given contour S is given by
= S B. dS.The change in this flux is given by
d/dt = S B/t - E. d,where the second term is due to Faraday’s law. If
the electric field is generated due to cross-field fluid motions, then, using Stokes’ theorem
E. d = S E. dS = S (v B). dS we see that
d/dt = S [B/t - (v B)] dS = S D 2B dS.
Thus, if D=0, the field is frozen in to the plasma; the flux through an area stays constant as the area deforms due to fluid motions. If, on the other hand, D 0, then the flux can change (and as a result the energy in the magnetic field can be released).
dΓE
B
dS
Φ
![Page 49: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/49.jpg)
Resistive DiffusionB/t = (v B) + D 2B
The magnetic flux through a given contour S is given by
= S B. dS.The change in this flux is given by
d/dt = S B/t - E. d,where the second term is due to Faraday’s law. If
the electric field is generated due to cross-field fluid motions, then, using Stokes’ theorem
E. d = S E. dS = S (v B). dS we see that
d/dt = S [B/t - (v B)] dS = S D 2B dS.
Thus, if D=0, the field is frozen in to the plasma; the flux through an area stays constant as the area deforms due to fluid motions. If, on the other hand, D 0, then the flux can change (and as a result the energy in the magnetic field can be released).
dΓE
B
dS
Φ
![Page 50: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/50.jpg)
Resistive DiffusionB/t = (v B) + D 2B
The ratio of the two terms on the RHS:(v B)/ D 2B ~ vL/D ~ 4vL/ηc2
is known as the magnetic Reynolds number S. For S >> 1, the plasma is essentially diffusion-free, for S <<1 the dynamics are driven by resistive diffusion.
For a flare loop, V ~ VA ~ 108 cm s-1, L ~ 109 cm andη ~ 10-7 T-3/2 ~ 10-17. This S ~ 1014, and the plasma should be almost perfectly frozen in.
The timescale for energy release should be of order L2/D ~ 4L2/ηc2 (this is of order the timescale for resistive decay of current in an inductor of inductance L/c2 and resistance R = ηL/L2 = η/L). For solar values, this is 1015 s ~ 107 years!
![Page 51: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/51.jpg)
Resistive DiffusionB/t = (v B) + D 2B
The ratio of the two terms on the RHS:(v B)/ D 2B ~ vL/D ~ 4vL/ηc2
is known as the magnetic Reynolds number S. For S >> 1, the plasma is essentially diffusion-free, for S <<1 the dynamics are driven by resistive diffusion.
For a flare loop, V ~ VA ~ 108 cm s-1, L ~ 109 cm andη ~ 10-7 T-3/2 ~ 10-17. This S ~ 1014, and the plasma should be almost perfectly frozen in.
The timescale for energy release should be of order L2/D ~ 4L2/ηc2 (this is of order the timescale for resistive decay of current in an inductor of inductance L/c2 and resistance R = ηL/L2 = η/L). For solar values, this is 1015 s ~ 107 years!
![Page 52: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/52.jpg)
Resistive DiffusionB/t = (v B) + D 2B
The ratio of the two terms on the RHS:(v B)/ D 2B ~ vL/D ~ 4vL/ηc2
is known as the magnetic Reynolds number S. For S >> 1, the plasma is essentially diffusion-free, for S <<1 the dynamics are driven by resistive diffusion.
For a flare loop, V ~ VA ~ 108 cm s-1, L ~ 109 cm andη ~ 10-7 T-3/2 ~ 10-17. This S ~ 1014, and the plasma should be almost perfectly frozen in.
The timescale for energy release should be of order L2/D ~ 4L2/ηc2 (this is of order the timescale for resistive decay of current in an inductor of inductance L/c2 and resistance R = ηL/L2 = η/L). For solar values, this is 1015 s ~ 107 years!
![Page 53: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/53.jpg)
Resistive DiffusionB/t = (v B) + D 2B
The ratio of the two terms on the RHS:(v B)/ D 2B ~ vL/D ~ 4vL/ηc2
is known as the magnetic Reynolds number S. For S >> 1, the plasma is essentially diffusion-free, for S <<1 the dynamics are driven by resistive diffusion.
For a flare loop, V ~ VA ~ 108 cm s-1, L ~ 109 cm andη ~ 10-7 T-3/2 ~ 10-17. This S ~ 1014, and the plasma should be almost perfectly frozen in.
The timescale for energy release should be of order L2/D ~ 4L2/ηc2 (this is of order the timescale for resistive decay of current in an inductor of inductance L/c2 and resistance R = ηL/L2 = η/L). For solar values, this is 1015 s ~ 107 years!
![Page 54: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/54.jpg)
Summary to Date
• Solar loops are big (they have a high inductance)
• Solar loops are good conductors• Solar loops have a low ratio of gas to
magnetic pressureSo:The plasma in solar loops is tied to the
magnetic field, and the motion of this field determines the motion of the plasma trapped on it
![Page 55: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/55.jpg)
Summary to Date
• Solar loops are big (they have a high inductance)
• Solar loops are good conductors• Solar loops have a low ratio of gas to
magnetic pressureSo:The plasma in solar loops is tied to the
magnetic field, and the motion of this field determines the motion of the plasma trapped on it
![Page 56: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/56.jpg)
Summary to Date
• Solar loops are big (they have a high inductance)
• Solar loops are good conductors• Solar loops have a low ratio of gas to
magnetic pressureSo:The plasma in solar loops is tied to the
magnetic field, and the motion of this field determines the motion of the plasma trapped on it
![Page 57: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/57.jpg)
Summary to Date
• Solar loops are big (they have a high inductance)
• Solar loops are good conductors• Solar loops have a low ratio of gas to
magnetic pressure βSo:The plasma in solar loops is tied to the
magnetic field, and the motion of this field determines the motion of the plasma trapped on it
![Page 58: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/58.jpg)
Summary to Date
• Solar loops are big (they have a high inductance)
• Solar loops are good conductors• Solar loops have a low ratio of gas to
magnetic pressure βSo:The plasma in solar loops is tied to the
magnetic field, and the motion of this field determines the motion of the plasma trapped on it
![Page 59: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/59.jpg)
Also:It is very difficult to release energy from such a high-conductivity, high-inductance system!
![Page 60: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/60.jpg)
Also:It is very difficult to release energy from such a high-conductivity, high-inductance system!
![Page 61: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/61.jpg)
Also:It is very difficult to release energy from such a high-conductivity, high-inductance system!
???
![Page 62: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/62.jpg)
The Vlasov Equation
Note that we have still prescribed E and B. A proper solution of the plasma equations requires that E and B be obtained self-consistently from the particle densities and currents. The equation that accounts for this is called the Vlasov equation.
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Phase-space Distribution FunctionThis is defined as the number of particles per unit
volume of space per unit volume of velocity space:
At time t, number of particles in elementary volume of space, with velocities in range v → v + dv = f(r,v,t) d3r d3v
f(r,v,t) has units cm-3 (cm s-1)-3
![Page 64: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/64.jpg)
The Boltzmann EquationThis equation expresses the fact that the net gain or
loss of particles in phase space is due to collisional depletion:
Df/Dt f/t + v.f + a.vf = (f/t)c
The Boltzmann equation takes into account the self-consistent evolution of the E and B fields through the appearance of the acceleration term a.
![Page 65: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/65.jpg)
The Vlasov Equation
This is a special case of the Boltzmann equation, with no collisional depletion term:
f/t + v.f + a.vf = 0,
i.e.,
f/t + v.f + (q/m) (E + (v/c) B).vf = 0.
![Page 66: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/66.jpg)
The Electrostatic Vlasov Equation
Setting B = 0, we obtain, in one dimension for simplicity, with q = -e (electrons)
f/t + v f/x - (eE/m) f/v = 0.
Perturb this around a uniform density, equilibrium (E = 0) state fo = ngo:
g1/t + v g1/x - (eE1/m) go/v = 0.
Also consider Poisson’s equation:
E1/x = 4ρ = - 4ne g1 dv
![Page 67: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/67.jpg)
The Electrostatic Vlasov Equation
Setting B = 0, we obtain, in one dimension for simplicity, with q = -e (electrons)
f/t + v f/x - (eE/m) f/v = 0.
Perturb this around a uniform density, equilibrium (E = 0) state fo = ngo:
g1/t + v g1/x - (eE1/m) go/v = 0.
Also consider Poisson’s equation:
E1/x = 4ρ = - 4ne g1 dv
![Page 68: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/68.jpg)
The Electrostatic Vlasov Equation
Setting B = 0, we obtain, in one dimension for simplicity, with q = -e (electrons)
f/t + v f/x - (eE/m) f/v = 0.
Perturb this around a uniform density, equilibrium (E = 0) state fo = ngo:
g1/t + v g1/x - (eE1/m) go/v = 0.
Also consider Poisson’s equation:
E1/x = 4ρ = - 4ne g1 dv
![Page 69: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/69.jpg)
The Electrostatic Vlasov Equation
Setting B = 0, we obtain, in one dimension for simplicity, with q = -e (electrons)
f/t + v f/x - (eE/m) f/v = 0.
Perturb this around a uniform density, equilibrium (E = 0) state fo = ngo:
g1/t + v g1/x - (eE1/m) go/v = 0.
Also consider Poisson’s equation (.E = 4):
E1/x = 4ρ = - 4ne g1 dv
![Page 70: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/70.jpg)
The Electrostatic Vlasov EquationNow consider modes of the form
g ~ exp(i[kx-ωt])Then the Vlasov equation becomes
-iωg1 + ivkg1 – (eE1/m) dgo/dv = 0
(ω – kv)g1 = (ieE1/m) dgo/dvand Poisson’s equation is
ikE1 = - 4ne g1 dvCombining,
ikE1= - i(4ne2/m) E1 dgo/dv dv/(ω – kv)
Simplifying, and defining the plasma frequency through ωpe2 =
4ne2/m,
1- (ωpe2/k2) dgo/dv dv/(v – ω/k) = 0.
This is the dispersion relation for electrostatic plasma waves.
![Page 71: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/71.jpg)
The Electrostatic Vlasov EquationNow consider modes of the form
g ~ exp(i[kx-ωt])Then the Vlasov equation becomes
-iωg1 + ivkg1 – (eE1/m) dgo/dv = 0
(ω – kv)g1 = (ieE1/m) dgo/dvand Poisson’s equation is
ikE1 = - 4ne g1 dvCombining,
ikE1= - i(4ne2/m) E1 dgo/dv dv/(ω – kv)
Simplifying, and defining the plasma frequency through ωpe2 =
4ne2/m,
1- (ωpe2/k2) dgo/dv dv/(v – ω/k) = 0.
This is the dispersion relation for electrostatic plasma waves.
![Page 72: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/72.jpg)
The Electrostatic Vlasov EquationNow consider modes of the form
g ~ exp(i[kx-ωt])Then the Vlasov equation becomes
-iωg1 + ivkg1 – (eE1/m) dgo/dv = 0
(ω – kv)g1 = (ieE1/m) dgo/dvand Poisson’s equation is
ikE1 = - 4ne g1 dvCombining,
ikE1= - i(4ne2/m) E1 dgo/dv dv/(ω – kv)
Simplifying, and defining the plasma frequency through ωpe2 =
4ne2/m,
1- (ωpe2/k2) dgo/dv dv/(v – ω/k) = 0.
This is the dispersion relation for electrostatic plasma waves.
![Page 73: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/73.jpg)
The Electrostatic Vlasov EquationNow consider modes of the form
g ~ exp(i[kx-ωt])Then the Vlasov equation becomes
-iωg1 + ivkg1 – (eE1/m) dgo/dv = 0
(ω – kv)g1 = (ieE1/m) dgo/dvand Poisson’s equation is
ikE1 = - 4ne g1 dvCombining,
ikE1= - i(4ne2/m) E1 dgo/dv dv/(ω – kv)
Simplifying, and defining the plasma frequency through ωpe2 =
4ne2/m,
1- (ωpe2/k2) dgo/dv dv/(v – ω/k) = 0.
This is the dispersion relation for electrostatic plasma waves.
![Page 74: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/74.jpg)
The Electrostatic Vlasov EquationNow consider modes of the form
g ~ exp(i[kx-ωt])Then the Vlasov equation becomes
-iωg1 + ivkg1 – (eE1/m) dgo/dv = 0
(ω – kv)g1 = (ieE1/m) dgo/dvand Poisson’s equation is
ikE1 = - 4ne g1 dvCombining,
ikE1= - i(4ne2/m) E1 dgo/dv dv/(ω – kv)
Simplifying, and defining the plasma frequency through ωpe2 =
4ne2/m,
1- (ωpe2/k2) dgo/dv dv/(v – ω/k) = 0.
This is the dispersion relation for electrostatic plasma waves.
![Page 75: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/75.jpg)
The Electrostatic Vlasov Equation
Integrating by parts, we obtain an alternative form
1- (ωpe2/ω2) go dv/(1 - kv/ω)2 = 0.
For a cold plasma, go = δ(v), so that we obtain
1- (ωpe2/ω2) = 0, i.e., ω = ωpe
![Page 76: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/76.jpg)
The Electrostatic Vlasov Equation
Integrating by parts, we obtain an alternative form
1- (ωpe2/ω2) go dv/(1 - kv/ω)2 = 0.
For a cold plasma, go = δ(v), so that we obtain
1- (ωpe2/ω2) = 0, i.e., ω = ωpe
![Page 77: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/77.jpg)
The Electrostatic Vlasov EquationFor a warm plasma, we expand the
denominator to get
1- (ωpe2/ω2) go dv[1 + 2kv/ω + 3k2v2/ω2 +
…] = 0
i.e. 1- (ωpe2/ω2) [1 + 3k2<v>2/ω2 + …] = 0,
where <v>2 = kBT/m is the average thermal speed. This gives the dispersion relation
ω2 = ωpe2 + 3 (kBT/m) k2
(cf. ω2 = ωpe2 + c2k2 for EM waves)
![Page 78: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/78.jpg)
The Electrostatic Vlasov EquationFor a warm plasma, we expand the
denominator to get
1- (ωpe2/ω2) go dv[1 + 2kv/ω + 3k2v2/ω2 +
…] = 0
i.e. 1- (ωpe2/ω2) [1 + 3k2<v>2/ω2 + …] = 0,
where <v>2 = kBT/m is the average thermal speed. This gives the dispersion relation
ω2 = ωpe2 + 3 (kBT/m) k2
(cf. ω2 = ωpe2 + c2k2 for EM waves)
![Page 79: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/79.jpg)
The Electrostatic Vlasov EquationFor a warm plasma, we expand the
denominator to get
1- (ωpe2/ω2) go dv[1 + 2kv/ω + 3k2v2/ω2 +
…] = 0
i.e. 1- (ωpe2/ω2) [1 + 3k2<v>2/ω2 + …] = 0,
where <v>2 = kBT/m is the average thermal speed. This gives the dispersion relation
ω2 = ωpe2 + 3 (kBT/m) k2
(cf. ω2 = ωpe2 + c2k2 for EM waves)
![Page 80: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/80.jpg)
The Electrostatic Vlasov EquationFor a warm plasma, we expand the
denominator to get
1- (ωpe2/ω2) go dv[1 + 2kv/ω + 3k2v2/ω2 +
…] = 0
i.e. 1- (ωpe2/ω2) [1 + 3k2<v>2/ω2 + …] = 0,
where <v>2 = kBT/m is the average thermal speed. This gives the dispersion relation
ω2 = ωpe2 + 3 (kBT/m) k2
(cf. ω2 = ωpe2 + c2k2 for EM waves)
![Page 81: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/81.jpg)
Dispersion relations
Electrostatic waves in a warm plasma:
ω2 = ωpe2 + 3 (kBTe/m) k2
Ion-acoustic waves (includes motion of ions):
ω = kcs; cs=[kB(Te + Ti)/mi]1/2
(note electrons effectively provide quasi-neutrality)
Upper hybrid waves (includes B):
ω2 = ωpe2 + Ωe
2; Ωe = eB/me
![Page 82: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/82.jpg)
Dispersion relations
Electrostatic waves in a warm plasma:
ω2 = ωpe2 + 3 (kBTe/m) k2
Ion-acoustic waves (includes motion of ions):
ω = kcs; cs=[kB(Te + Ti)/mi]1/2
(note electrons effectively provide quasi-neutrality)
Upper hybrid waves (includes B):
ω2 = ωpe2 + Ωe
2; Ωe = eB/me
![Page 83: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/83.jpg)
Dispersion relations
Electrostatic waves in a warm plasma:
ω2 = ωpe2 + 3 (kBTe/m) k2
Ion-acoustic waves (includes motion of ions):
ω = kcs; cs=[kB(Te + Ti)/mi]1/2
(note electrons effectively provide quasi-neutrality)
Upper hybrid waves (includes B):
ω2 = ωpe2 + Ωe
2; Ωe = eB/me
![Page 84: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/84.jpg)
Dispersion relations
Electrostatic waves in a warm plasma:
ω2 = ωpe2 + 3 (kBTe/m) k2
Ion-acoustic waves (includes motion of ions):
ω = kcs; cs=[kB(Te + Ti)/mi]1/2
(note electrons effectively provide quasi-neutrality)
Upper hybrid waves (includes B):
ω2 = ωpe2 + Ωe
2; Ωe = eB/me
![Page 85: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/85.jpg)
Dispersion relations
Alfvén waves:
ω2 = k2VA2/[1 + (VA
2/c2)]
Magnetoacoustic waves:
ω4 - ω2k2(cs2 + VA
2) + cs2VA
2k4cos2θ = 0
(θ = angle of propagation to magnetic field)
etc., etc.
![Page 86: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/86.jpg)
Dispersion relations
Alfvén waves:
ω2 = k2VA2/[1 + (VA
2/c2)]
Magnetoacoustic waves:
ω4 - ω2k2(cs2 + VA
2) + cs2VA
2k4cos2θ = 0
(θ = angle of propagation to magnetic field)
etc., etc.
![Page 87: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/87.jpg)
Dispersion relations
Alfvén waves:
ω2 = k2VA2/[1 + (VA
2/c2)]
Magnetoacoustic waves:
ω4 - ω2k2(cs2 + VA
2) + cs2VA
2k4cos2θ = 0
(θ = angle of propagation to magnetic field)
etc., etc.
![Page 88: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/88.jpg)
Two-Stream Instability1- (ωpe
2/ω2) go dv/(1 - kv/ω)2 = 0.For two streams,
go = [δ(v-U) + δ(v+U)],so that
(ωpe2/[ω-kU]2) + (ωpe
2/[ω+kU]2) = 1.
This is a quadratic in ω2:
ω4 – 2(ωpe2 + k2U2)ω2 – 2 ωpe
2k2U2 + k4U4 = 0,with solution
ω2 = (ωpe2 + k2U2) ωpe (ωpe
2 + 4k2U2)1/2
There are solutions with ω2 negative and so imaginary (exponentially growing) solutions.
![Page 89: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/89.jpg)
Two-Stream Instability1- (ωpe
2/ω2) go dv/(1 - kv/ω)2 = 0.For two streams,
go = [δ(v-U) + δ(v+U)],so that
(ωpe2/[ω-kU]2) + (ωpe
2/[ω+kU]2) = 1.
This is a quadratic in ω2:
ω4 – 2(ωpe2 + k2U2)ω2 – 2 ωpe
2k2U2 + k4U4 = 0,with solution
ω2 = (ωpe2 + k2U2) ωpe (ωpe
2 + 4k2U2)1/2
There are solutions with ω2 negative and so imaginary (exponentially growing) solutions. U-U
g
v
![Page 90: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/90.jpg)
Two-Stream Instability1- (ωpe
2/ω2) go dv/(1 - kv/ω)2 = 0.For two streams,
go = [δ(v-U) + δ(v+U)],so that
(ωpe2/[ω-kU]2) + (ωpe
2/[ω+kU]2) = 1.
This is a quadratic in ω2:
ω4 – 2(ωpe2 + k2U2)ω2 – 2 ωpe
2k2U2 + k4U4 = 0,with solution
ω2 = (ωpe2 + k2U2) ωpe (ωpe
2 + 4k2U2)1/2
There are solutions with ω2 negative and so imaginary (exponentially growing) solutions. U-U
g
v
![Page 91: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/91.jpg)
Two-Stream Instability1- (ωpe
2/ω2) go dv/(1 - kv/ω)2 = 0.For two streams,
go = [δ(v-U) + δ(v+U)],so that
(ωpe2/[ω-kU]2) + (ωpe
2/[ω+kU]2) = 1.
This is a quadratic in ω2:
ω4 – 2(ωpe2 + k2U2)ω2 – 2 ωpe
2k2U2 + k4U4 = 0,with solution
ω2 = (ωpe2 + k2U2) ωpe (ωpe
2 + 4k2U2)1/2
There are solutions with ω2 negative and so imaginary (exponentially growing) solutions. U-U
g
v
![Page 92: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/92.jpg)
Two-Stream Instability
Distribution with two maxima (one at zero, one at the velocity of the “beam”) is susceptible to the two-stream instability.
This generates a large amplitude of plasma waves and affects the energetics of the particles.
![Page 93: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/93.jpg)
Two-Stream Instability
This can also happen due to an “overtaking” instability – fast particles arrive at a location earlier than slower ones and so create a local maximum in f.
![Page 94: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/94.jpg)
Summary
High energy solar physics is concerned with the physics of plasma, which is a highly interacting system of particles and waves.
![Page 95: Basic Plasma Physics Principles Gordon Emslie Oklahoma State University.](https://reader036.fdocuments.in/reader036/viewer/2022070308/551c4c395503467b488b504e/html5/thumbnails/95.jpg)
Summary
High energy solar physics is concerned with the physics of plasma, which is a highly interacting system of particles and waves.
“Plasma physics is complicated” (J.C. Brown & D.F. Smith, 1980)