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Hydromagnetic stability of a rotating baroclinic star

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Abstract

The magnetohydrodynamic stability of rotating baroclinic star has been studied in the presence of poloidal and toroidal magnetic fields taking into account the diffusive effects. Necessary conditions for stability have been found by normal mode analysis under small wavelength approximation.

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References

  • Busse, F. H.: 1981,Geophys. Astrophys. Fluid Dyn. 17, 215.

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  • Tassoul, J. L.: 1978,Theory of Rotating Stars, Princeton Univ. Press.

  • Zahn, J. P.: 1974, in P. Ledoux, A. Noels, and A. W. Rodgers (eds.), ‘Stellar Instability and Evolution’,IAU Symp. 59, 185.

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Authors and Affiliations

  1. Department of Mathematics, Bharathiar University, Coimbatore, India

    M. R. Raghavachar

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  1. M. R. Raghavachar
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Raghavachar, M.R. Hydromagnetic stability of a rotating baroclinic star. Astrophys Space Sci 100, 85–93 (1984). https://doi.org/10.1007/BF00651587

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  • DOI: https://doi.org/10.1007/BF00651587

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