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An illustration of the structure of the Sun and a red giant star, showing their convective zones. These are the granular zones in the outer layers of the stars. A convection zone, convective zone or convective region of a star is a layer which is unstable due to convection. Energy is primarily or partially transported by convection in such
Stellar structure models describe the internal structure of a star in detail and make predictions about the luminosity, the color and the future evolution of the star. Different classes and ages of stars have different internal structures, reflecting their elemental makeup and energy transport mechanisms.
An illustration of the structure of the Sun and a red giant star, showing their convective zones. These are the granular zones in the outer layers of these stars. The convection zone of a star is the range of radii in which energy is transported outward from the core region primarily by convection rather than radiation.
This diagram shows a cross-section of a Sun-like star, showing the internal structure. ... Convection is a more efficient mode for carrying energy than radiation, but ...
This core convection occurs in stars where the CNO cycle contributes more than 20% of the total energy. As the star ages and the core temperature increases, the region occupied by the convection zone slowly shrinks from 20% of the mass down to the inner 8% of the mass. [25] The Sun produces on the order of 1% of its energy from the CNO cycle.
Star formation is the process by ... The combination of convection within the protostar ... Star-forming region S106. The structure of the molecular cloud and ...
The first ever close-up picture of a star outside of our galaxy has shown that it is wrapped in a strange structure. The image shows a star named WOH G64 that is surrounded by gas and dust.
Differences in structure between a star on the main sequence, on the red giant branch, and on the horizontal branch. Once the supply of hydrogen at the core of a low-mass star with at least 0.25 M ☉ [8] is depleted, it will leave the main sequence and evolve along the red giant branch of the Hertzsprung–Russell diagram.