Abstract
Using an unrestricted second order virial tensor analysis, the characteristic frequencies of small adiabatic oscillations of a convective stellar model in the presence of a weak poloidal magnetic field, with significant radiation pressure, have been calculated. In the absence of the magnetic field, the effect of increase in radiation pressure is to decrease the frequencies of radial modes, in spite of the increase in central condensation of the system. The characteristic frequencies of the transverse shear mode, the toroidal mode, and the pulsation modes show a general increase with the increase in the field strength. The marginal stability of the configuration in the presence of the magnetic field has also been discussed.
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