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The convective zone,energy is transferred much faster that it is in the radiative zone.
In the radiative zone, energy moves from atom to atom in the form of electromagnetic waves, or radiation. Energy produced in the core moves through this zone by convection, the transfer of energy by moving liquids or gases.
In both cases, heat is transferred via convection.
Carbon does not transfer via radiation. Carbon can only "conduct" in the sense that it can diffuse through a solid if the temperature is high enough. Carbon can convect in convective models, and the analyses of both heat transfer and mass transfer in solid surface - fluid mediums are *very* similar.
The Radiative Zone.
The convective zone,energy is transferred much faster that it is in the radiative zone.
The convective zone,energy is transferred much faster that it is in the radiative zone.
The convective zone,energy is transferred much faster that it is in the radiative zone.
From the Sun's core, energy moves through the radiative zone, across the tachocline (transition layer) to the convective zone, and then to the outer convective zone with its visible granulation.
In the radiative zone, energy moves from atom to atom in the form of electromagnetic waves, or radiation. Energy produced in the core moves through this zone by convection, the transfer of energy by moving liquids or gases.
Carries energy upward by convection.
In the radiative zone, energy moves from atom to atom in the form of electromagnetic waves, or radiation. Energy produced in the core moves through this zone by convection, the transfer of energy by moving liquids or gases.
No
it does
The Sun's radiative zone is the section of the solar interior between the innermost core and the outer convective zone. In the radiative zone, energy generated by nuclear fusion in the core moves outward as electromagnetic radiation. In other words, the energy is conveyed by photons. When the energy reaches the top of the radiative zone, it begins to move in a different fashion in the convective zone. In the convective zone, heat and energy are carried outward along with matter in swirling flows called convection cells. This motion is similar to the roiling flows seen in a pot of boiling water. The inner parts of the Sun (core and radiative zone) spin differently than the outer layers (convective zone). The boundary between these two types of rotation, which lies between the radiative and convective zones, is called the tachocline. Many other stars also have radiative zones. The Sun's radiative zone extends from the core outward to about 70% of the Sun's radius. In a smaller (than the Sun) star that is cooler than our Sun, the convective zone tends to be larger, extending deeper into the star's interior. Thus the radiative zone tends to be smaller. In very small, cool stars the convective zone may reach all the way to the star's core, and there may be no radiative zone at all. In a larger (than the Sun) star with a higher temperature, the radiative zone tends to be larger and the convective zone smaller. Especially large, hot stars may not have a convective zone at all - their radiative zone may extend all the way from the core to the star's surface.
A convection zone is the final process of the sun's radius. Energy from the sun is carried outward to the surface by convection currents.
The radiation zone is the "middle part" of the interior of the Sun. It is adjacent to the core. In this zone, energy travels between the atoms as photons of gamma radiation. Above the radiative zone is the convective zone. Scientists estimate that core energy takes as long as 170,000 years to travel through the dense matter of the radiative zone.According to NASA, the Sun's radiative zone begins about 108,125 miles from the center of the Sun and ends about 302,750 miles from the center of the sun.In some stars, it is believed that the layering is reversed, with the inner layer convective and the outer layers radiative.