Written by an international team of astrophysicists (affiliated with the Leibniz Institute of Astrophysics in Potsdam, the Institute of Solar-Terrestrial Physics in Irkutsk and the Institute of Geophysics at ETH Zurich), this volume tackles the difficult subject of the role of magnetohydrodynamical
processes in the physics of stellar formation and evolution, and touches upon larger-scale processes in the interstellar medium, including galactic dynamics.
This is most often realized by means of the so-called ideal magnetohydrodynamical
equations, where various ions are treated as a single fluid, the conductivity of the ionised gas is assumed to be very large and the plasma is assumed to be frozen in the magnetic field.
The theory proves: the motion of a magnetohydrodynamical
, electro-hydrodynamical or hydrodynamical incompressible fluid is locally unstable everywhere relative to the disturbances of a vortex, magnetic or electric held.
For example, magnetohydrodynamical
pipe flow may lead to the convection-diffusion equation (1.1) with b = (1, 0) and [u.sub.b] = 0; cf., e.g., .
The first represents the coronal magnetic loops and flux tubes as resonators and waveguides for magnetohydrodynamical
oscillations and waves.