Understanding Alfvén Velocity
The Alfvén velocity is the speed at which Alfvén waves — transverse oscillations of magnetic field lines — propagate through a magnetized, electrically conducting plasma. Named after Swedish physicist Hannes Alfvén, who first described them in 1942 and received the 1970 Nobel Prize in Physics largely for this work, these waves are fundamental to solar wind physics, planetary magnetospheres, the solar corona, and magnetically confined fusion plasmas.
The formula
The Alfvén velocity is defined as vA = B / √(μ₀ρ), where B is the magnetic field strength in tesla, μ₀ is the vacuum permeability (4π×10⁻⁷ T·m/A), and ρ is the plasma mass density in kg/m³. Because mass density is rarely measured directly, it is usually derived from particle number density: ρ = n × A × mᵤ, where n is the number density, A is the mean ion mass number (1 for hydrogen or protons, 4 for helium, and so on), and mᵤ is the atomic mass unit (1.6605×10⁻²⁷ kg).
Plasma beta and wave dominance
Plasma beta, β = 2μ₀nk_BT/B², compares thermal (particle) pressure to magnetic pressure. When β is well below 1, the magnetic field dominates and Alfvén waves are the primary way disturbances travel through the plasma. When β exceeds 1, thermal pressure dominates and compressive, sound-like waves become more important than Alfvén waves.
Getting accurate results
- Measure or estimate the magnetic field, particle density, and temperature at the same location and time — Alfvén speed varies enormously between environments (tens of km/s in the solar wind, thousands of km/s in the solar corona).
- Choose the ion species that dominates the plasma's mass. For a hydrogen or proton-electron plasma use A = 1; heavier ions such as helium or oxygen noticeably lower the Alfvén speed at the same number density.
- Remember the formula is non-relativistic: in extreme environments such as pulsar or magnetar magnetospheres, the classical result can approach or exceed the speed of light, where a relativistic correction becomes necessary.