Linear r-Modes below the Sun's Convective Envelope

Details Linear r-Modes below the Sun's Convective Envelope Linear r-Modes below the Sun's Convective Envelope

Mar 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000apj...531..591w&link_type=abstract

The Astrophysical Journal, Volume 531, Issue 1, pp. 591-598.

Astronomy and Astrophysics

Astronomy

8

Convection, Hydrodynamics, Stars: Oscillations, Sun: Interior, Sun: Oscillations

Scientific paper

Theoretical properties of linear r-modes in a standard solar interior are computed, and the excitation of some by convective overshoot is estimated. The modes oscillate in a resonant cavity usually occupying most of the nonconvecting interior. Most modes concentrate their kinetic energy toward the center of the Sun. Over half the energy usually lies below 0.15 Rsolar with an asymptotic limit of 0.11 Rsolar for high radial harmonics (Rsolar is the solar radius). The oscillation frequencies are very close to the well-known toroidal frequency, σt=2Ωm[l(l+1)]-1, deviating by fractional amounts ~10-6+/-1 which are roughly 3 orders of magnitude smaller than deviations found earlier for r-modes in convective layers. An explicit formula for the ratio of divergent motion to curl motion is derived. It shows how rapidly the compressible component changes as a function of r. Compressibility is only ~10-6 of the total motion for low l-modes and declines proportionally to ml-3 for high l. A small subset of modes (the lowest radial harmonic of angular states |m|=l) avoid the core which makes them sensitive to convective overshoot. Just one of the giant convection cells detected by Beck et al. can excite such modes to kilometer-size amplitudes with the possibility that far larger displacement amplitudes can accumulate in the mode over time if the interaction between cells and r-modes is found to be strong.

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