http://wiki.keithl.com/SolarWind
Basics of the Solar Wind
Nicole Meyer-Vernet PSULib QB529.M485 2007
Observatoire de Paris and Centre National de la Rechereche Scientifique website
- p009 Sun: mass 1.98892e30 kg, radius 695700 km, Luminosity 3.828e26 W +/-0.1%
- p054 plasmas interact less with radiation than with plasmas
p057 Fermi energy
book's "comet-like" heliosphere model obsolete
Imaging the Interaction of the Heliosphere with the Interstellar Medium from Saturn with Cassini
- p057 plasma particle collisional free path increases strongly with speed, fast particles nearly collisionless
- p064 Magnetic mirrors: particle moving towards converging/increasing field mirrors and reflects
- p066 transverse gradient produces a small transverse drift
p080 "upstream kinetic energy converted to downstream enthalpy, high temperature
- p083 viscous forces generally much less important than inertial effects, but
see E. M. Purcell Life at low Reynolds number Am. J. Phys. 45, 3–11 (1977)
- p083 ions transport momentum, determining viscosity; electrons transport heat, determining thermal conductivity
- p084 Reynolds number very large for space plasmas, viscosity generally negligable
- p084 1e6 K (kelvin) solar corona heat conductivity 1e4 W/m-K "same order of magnitude as brass"
NO, brass approx. 150 W/m-K Silver around 430 W/m-K
- p084 conductivity low perpendicular to B, high parallel to B only if mean free path much smaller than scales of variation.
p088 magnetic Reynolds number convection ÷ diffusion
p090 magnetic field freezing Alfvén's theorem
- p090 plasmas in space tied to field lines, do not mix across field
- p091 magnetized plasma has
- inertia, corresponding to bulk kinetic energy ½ρV²
- thermal pressure, corresponding to random kinetic energy ρkT/m
- magnetic forces, corresponding to B²/2μ₀
p092 V = B/(μ₀ρ)½ ≡ VA Alfvén speed
