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This combination of circumstances produces an outer convection zone, the top of which is visible in the Sun as solar granulation. Low-mass main-sequence stars, such as red dwarfs below 0.35 solar masses, [3] as well as pre-main sequence stars on the Hayashi track, are convective throughout and do not contain a radiation zone. [4]
The Sun in the middle has an inner radiating zone and an outer convective zone. The radiative zone is the thickest layer of the Sun, at 0.45 solar radii. From the core out to about 0.7 solar radii , thermal radiation is the primary means of energy transfer. [ 74 ]
In the Sun, the region between the solar core at 0.2 of the Sun's radius and the outer convection zone at 0.71 of the Sun's radius is referred to as the radiation zone, although the core is also a radiative region. [1] The convection zone and the radiative zone are divided by the tachocline, another part of the Sun.
The Solar Orbiter mission has captured the highest-resolution views of the sun’s ... Rippling beneath the photosphere layer is hot plasma that shifts around in the sun’s convection zone ...
In solar physics and observation, granules are convection cells in the Sun's photosphere. They are caused by currents of plasma in the Sun's convective zone, directly below the photosphere. The grainy appearance of the photosphere is produced by the tops of these convective cells; this pattern is referred to as granulation.
From there they cross into the convective zone (the remaining 25% of distance from the Sun's center), where the dominant transfer process changes to convection, and the speed at which heat moves outward becomes considerably faster. [14]
For example, in the Sun the convection at the base of the convection zone, near the core, is adiabatic but that near the surface is not. The mixing length theory contains two free parameters which must be set to make the model fit observations, so it is a phenomenological theory rather than a rigorous mathematical formulation.
This suggests that the convective zone alone may be responsible for the function of the solar dynamo. [1] The term tachocline was coined in a paper by Edward Spiegel and Jean-Paul Zahn in 1992 [2] by analogy to the oceanic thermocline. An illustration of the structure of the Sun