Gravity Waves in the Sun

Tamara M. Rogers; Gary A. Glatzmaier

doi:10.1111/j.1365-2966.2005.09659.x

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arXiv · astro-ph/0508560

Gravity Waves in the Sun

Tamara M. Rogers·Gary A. Glatzmaier

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Abstract

We present numerical simulations of penetrative convection and gravity wave excitation in the Sun. Gravity waves are self-consistently generated by a convective zone overlying a radiative interior. We produce power spectra for gravity waves in the radiative region as well as estimates for the energy flux of gravity waves below the convection zone. We calculate a peak energy flux in waves below the convection zone to be three orders of magnitude smaller than previous estimates for m=1. The simulations show that the linear dispersion relation is a good approximation only deep below the convective-radiative boundary. Both low frequency propagating gravity waves as well as higher frequency standing modes are generated; although we find that convection does not continually drive the standing g-mode frequencies.

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Tamara M. Rogers, Gary A. Glatzmaier. 2005-08-25. Gravity Waves in the Sun. https://doi.org/10.1111/j.1365-2966.2005.09659.x

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