Astronomy and astrophysics Definition
Parker instability
Builds on MagnetohydrodynamicsMagnetic fieldHydrostatic equilibrium
Definition
Consider a perfectly conducting gas in a uniform gravitational field with , governed by ideal magnetohydrodynamics. Let the gas be in a static equilibrium stratified in the height , with a horizontal magnetic field . In this equilibrium the gas pressure and the magnetic pressure together balance gravity, as in hydrostatic equilibrium. The Parker instability is the linear instability of this equilibrium to perturbations that bend the field lines in the vertical plane. In the growing perturbation, gas flows along the field lines from the crests into the troughs, and the crests rise by buoyancy.
Remarks
Example: in an isothermal layer with a constant ratio of magnetic to gas pressure, the equilibrium density falls off exponentially with height, and perturbations of long enough horizontal wavelength grow. Non-example: an isothermal layer with no magnetic field, supported by gas pressure alone, is convectively stable and shows no Parker instability. The instability needs the field to carry part of the weight. Perturbations that vary only across the field, without bending it, are called interchange modes; the Parker instability refers to the undular modes along the field. The cosmic rays of the galaxy add a pressure tied to the field and strengthen the instability.
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Further reading
About this page
| Tag | T65B79VD3F |
|---|---|
| URI | m2://T65B79VD3F |
| Kind | definition |
| Writing | W0 stub |
| MSC | 85A30, 76E25, 76W05 |
| Defines | Parker instability |
| Uses | Magnetohydrodynamics, Magnetic field, Hydrostatic equilibrium |
| Changed | 3 November 2026 |
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