Adiabatic pulsations and convective instability of rotating gaseous masses. II Differential rotation and toroidal magnetic fields

Details Adiabatic pulsations and convective instability of rotating gaseous masses. II Differential rotation and toroidal magnetic fields Adiabatic pulsations and convective instability of rotating gaseous masses. II Differential rotation and toroidal magnetic fields

Dec 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974ap%26ss..31..449k&link_type=abstract

Astrophysics and Space Science, vol. 31, Dec. 1974, p. 449-475.

Astronomy and Astrophysics

Astrophysics

5

Astronomical Models, Harmonic Oscillation, Stellar Magnetic Fields, Stellar Rotation, Thermal Instability, Virial Theorem, Adiabatic Conditions, Convective Flow, Dynamic Stability, Magnetic Field Configurations, Velocity Distribution

Scientific paper

Third order virial equations have been used to investigate the oscillations and the stability of the sequence of differentially rotating, compressible Maclaurin spheroids in the presence of toroidal magnetic fields. It is shown that the neutral point occurring at eccentricity e = 0.731 13, which is the analogue of the first point of bifurcation along the Dedekind sequence, remains unaffected by the presence of differential rotation or a toroidal magnetic field. The point of onset of dynamical instability corresponding to the third harmonic deformations does, however, depend upon the magnetic field. It is shifted to values higher than e = 0.966 96, the value that obtains in the case of uniform rotation; and a sufficiently large magnetic field can suppress this point. Complete frequency spectra are obtained in two cases of interest: when the equilibrium state is one of equipartition, and when toroidal magnetic and velocity fields (vanishing at the surface) are present in a configuration rotating with a constant angular velocity.

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