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Self-consistent models of the magnetospheric structure of rapidly
rotating stars
Richard Ryan (St. Andrews)
We present a method for modelling the magnetospheric structure of rapidly
rotating stars. The models are based on stationary solutions of the ideal
MHD equations for a parallel rotator using axisymmetry. We focus
especially on the regions of closed field lines with trapped co-rotating
plasma. The resulting non-linear equilibrium equation is solved by a
numerical continuation method developed to follow the bifurcation, limit
and catastrophe points of equilibrium sequences as prescribed model
parameters like the rotation rate or the pressure at the coronal base are
changed. We will present some representative results for a first simple
model using the assumption of an isothermal plasma and discuss them in the
light of observations.
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