Differential rotation of the Sun Differential rotation



internal rotation in sun, showing differential rotation in outer convective region , uniform rotation in central radiative region.



on sun, study of oscillations revealed rotation constant within whole radiative interior , variable radius , latitude within convective envelope. sun has equatorial rotation speed of ~2 km/s; differential rotation implies angular velocity decreases increased latitude. poles make 1 rotation every 34.3 days , equator every 25.05 days, measured relative distant stars (sidereal rotation).


the highly turbulent nature of solar convection , anisotropies induced rotation complicate dynamics of modeling. molecular dissipation scales on sun @ least 6 orders of magnitude smaller depth of convective envelope. direct numerical simulation of solar convection have resolve entire range of scales in each of 3 dimensions. consequently, solar differential rotation models must involve approximations regarding momentum , heat transport turbulent motions not explicitly computed. thus, modeling approaches can classified either mean-field models or large-eddy simulations according approximations.







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