Inertial oscillations in the solar convection zone. I - Spherical shell model

Details Inertial oscillations in the solar convection zone. I - Spherical shell model Inertial oscillations in the solar convection zone. I - Spherical shell model

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...295..195g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 295, Aug. 1, 1985, p. 195-212.

Astronomy and Astrophysics

Astrophysics

9

Convective Flow, Coriolis Effect, Solar Oscillations, Stellar Cores, Continuity Equation, Eigenvalues, Finite Difference Theory, Solar Interior, Stream Functions (Fluids)

Scientific paper

The solar oscillation spectrum has the potential to provide a great deal of information about the sun's interior. However, an interpretation of the oscillation spectrum is an extremely difficult task. Neither direct nor indirect approaches can give a complete picture of the solar interior. It appears, therefore, advisable to employ a wide variety of methods to probe the sun's interior. In the present paper, a description is provided of a family of solar oscillations, which is called inertial oscillations. It is shown that these oscillations are sensitive (independently) to both the depth and the rotation profile of the convection zone. If these modes can be observed, they will provide an independent determination of the convection zone depth and rotation frequency profile, as a function of radius (and latitude).

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