Inertial oscillations in the solar convection zone. II - A cylindrical model for equatorial regions

Details Inertial oscillations in the solar convection zone. II - A cylindrical model for equatorial regions Inertial oscillations in the solar convection zone. II - A cylindrical model for equatorial regions

Sep 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...296..685g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 296, Sept. 15, 1985, p. 685-695.

Statistics

Computation

3

Convection, Solar Oscillations, Solar Rotation, Computational Astrophysics, Cylindrical Shells, Equatorial Regions, Inertia, Spherical Shells, Stellar Models, Stellar Structure

Scientific paper

Axisymmetric inertial oscillations found from a simplified, cylindrical model applicable to equatorial latitudes are presented and compared to results obtained previously by numerical methods for a spherical shell. The asymptotic behavior of inertial mode frequencies are analytically derived in the limits of very large and very small axial wavenumbers, and it is shown that inertial oscillations arise only when the angular momentum per unit mass increases outward. The effects of convection zone depth and differential rotation on the different radial orders of inertial modes are demonstrated. In a convection zone 15 billion cm in depth, rotation rate increasing inward leads to decreased oscillation frequency for a given radial order and axial wavenumber, the opposite of the result for a spherical shell. Deeper zones in the cylindrical case give increased frequencies for rotation rate either decreasing or increasing inward. The differences in the results between spherical and cylindrical models are shown to be due to the different geometries.

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