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 ...
– As particles bounce they will drift because of gradient and curvature drift motion. – If the field is a dipole their trajectories will take them around the planet and close on themselves. • The third adiabatic invariant – As long as the magnetic field doesn’t change much in the time required to drift around a rplanet the magnetic flux Φ = ∫ B ⋅ nˆ dA inside the orbit must be constant. – Note it is the total flux that is conserved including the flux within the planet.
- 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 26 and 27: • Limitations on the invariants
- Page 28 and 29: - Average random energy r r 2 − =
- Page 30 and 31: - Other frequently used distributio
- Page 32: ϕ = −r λ qe D 4π ε 0 r •The
- Page 35 and 36: - The frequency of this oscillation
- Page 37 and 38: • Magnetohydrodynamics (MHD) - Th
- Page 39 and 40: u s ⋅∇ u s 0 - The term means t
- Page 41: • Maxwell’s equations r ∂B r
- 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
– As particles bounce they will drift<br />
because <strong>of</strong> gradient and<br />
curvature drift motion.<br />
– If the field is a dipole their<br />
trajec<strong>to</strong>ries will take them around<br />
the planet and close on<br />
themselves.<br />
• The third adiabatic invariant<br />
– As long as the magnetic field<br />
doesn’t change much in the time<br />
required <strong>to</strong> drift around a rplanet<br />
the magnetic flux Φ = ∫ B ⋅ nˆ<br />
dA<br />
inside the orbit must be constant.<br />
– Note it is the <strong>to</strong>tal flux that is<br />
conserved including the flux<br />
within the planet.
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