A Brief Introduction to Space Plasma Physics.pdf - Institute of ...
A Brief Introduction to Space Plasma Physics.pdf - Institute of ... A Brief Introduction to Space Plasma Physics.pdf - Institute of ...
– Often the last terms on the right in Ohm’s Law can be dropped – If the plasma is collisionless, may be very large so • Frozen in flux r r r r J = σ ( E + u × B) σ r r r E + u × B = 0 – Combining Faraday’s law ( ), and r ∇× B Ampere’ law ( ) with r ∂B ∂t η m = 1 σ µ 0 r r ∂B ∇× E = − r r ∂rt r r = µ 0 J J = σ ( E + u × B) r r r 2 = ∇× ( u × B) + η ∇ B where is the magnetic viscosity – If the fluid is at rest this rbecomes a “diffusion” equation ∂B r 2 = ηm∇ B ∂t – The magnetic field will exponentially decay (or diffuse) from a 2 conducting medium in a time τ D = L η where L B is the system size. m B m
- Page 1 and 2: ESS 200C - Space Plasma Physics Win
- Page 3 and 4: Space Plasma Physics • Space phys
- Page 5 and 6: - Galileo theorized that aurora is
- Page 7 and 8: The Plasma State • A plasma is an
- Page 9 and 10: • B acts to change the motion of
- Page 11: • The electric field can modify t
- Page 14 and 15: • The change in the direction of
- Page 16 and 17: • Maxwell’s equations - Poisson
- Page 18 and 19: • Maxwell’s equations in integr
- Page 20 and 21: • For a coordinate in which the m
- Page 22 and 23: B r • The force is along and away
- Page 24: - As particles bounce they will dri
- Page 27 and 28: The Properties of a Plasma • A pl
- Page 29 and 30: • For monatomic particles in equi
- Page 31 and 32: • What makes an ionized gas a pla
- Page 34 and 35: • The plasma frequency - Consider
- Page 36 and 37: • A note on conservation laws - C
- Page 38 and 39: - Momentum equation r ∂us r r r r
- Page 40 and 41: • Energy equation ∂ ( ∂t 1 2
- Page 44 and 45: - On time scales much shorter than
- Page 46 and 47: 2 - bˆ B ⋅∇B ˆ ˆ∇B cancels
- Page 48 and 49: • The exponent gives the phase of
- Page 50 and 51: • MHD waves - natural wave modes
- Page 52 and 53: ∂p ∂x • Since = 0 , = 0 and =
- Page 54 and 55: • Compressible solutions - In gen
- Page 56 and 57: - For a plane wave solution - The d
- Page 58 and 59: • Alfven waves propagate parallel
– Often the last terms on the right in Ohm’s Law can be dropped<br />
– If the plasma is collisionless, may be very large so<br />
• Frozen in flux<br />
r r r r<br />
J = σ ( E + u × B)<br />
σ<br />
r r r<br />
E + u × B = 0<br />
– Combining Faraday’s law ( ), and<br />
r<br />
∇× B<br />
Ampere’ law ( ) with<br />
r<br />
∂B<br />
∂t<br />
η<br />
m<br />
= 1 σ µ 0<br />
r<br />
r ∂B<br />
∇× E = −<br />
r r ∂rt<br />
r r<br />
= µ 0<br />
J J = σ ( E + u × B)<br />
r r r<br />
2<br />
= ∇× ( u × B)<br />
+ η ∇ B<br />
where is the magnetic viscosity<br />
– If the fluid is at rest this rbecomes a “diffusion” equation<br />
∂B<br />
r<br />
2<br />
= ηm∇<br />
B<br />
∂t<br />
– The magnetic field will exponentially decay (or diffuse) from a<br />
2<br />
conducting medium in a time τ D<br />
= L η where L B<br />
is the system size.<br />
m<br />
B<br />
m
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