Linear modes of convection in the solar envelope

Details Linear modes of convection in the solar envelope Linear modes of convection in the solar envelope

Feb 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...236..285b&link_type=abstract

Astrophysical Journal, Part 1, vol. 236, Feb. 15, 1980, p. 285-293.

Physics

10

Convective Heat Transfer, Mixing Length Flow Theory, Propagation Modes, Solar Physics, Stellar Envelopes, Flow Velocity, Inviscid Flow, Linear Systems, Solar Granulation, Stellar Models

Scientific paper

The structure of the solar convective envelope calculated according to mixing-length theory is not consistent with the transport of the convective heat flux by any superposition of the fundamental linear convective modes. If the amplitudes of these modes can be estimated by consideration of the most important nonlinear terms in the equations of motion, it becomes possible to find solar models which are consistent with mode transport of the heat through the convective zone. These models may be characterized by a mixing length which varies from point to point through the envelope. The linear modes in such models show peaks in velocity at certain preferred length scales, but these scales do not necessarily correspond to those of the solar motions, such as the supergranulation.

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