It is the radiation of heat.
The radiative zone is hotter than the convection zone. In the radiative zone, energy is transferred through electromagnetic radiation, while in the convection zone, energy is transferred through the movement of hot gas or plasma.
An object is in radiative balance when it absorbs the same amount of radiation as it emits. This equilibrium results in a steady temperature for the object.
The radiative zone extends from the outer edge of the solar core to about 70% of the distance to the solar surface. It is approximately 200,000 kilometers thick.
Oh, dude, photons are like the rockstars of the Sun, cruising through the radiative zone at the speed of light. It takes them about a million years to make their way from the core to the convective zone. So, you know, just your average cosmic commute.
The convection zone.
Radiative energy is carried by light.
The radiative zone is hotter than the convection zone. In the radiative zone, energy is transferred through electromagnetic radiation, while in the convection zone, energy is transferred through the movement of hot gas or plasma.
yes
The radiative zone of the Sun is not visible to the human eye, so it does not have a color. It is located beneath the Sun's visible surface where energy is transported by photons through a process of radiative diffusion.
An object is in radiative balance when it absorbs the same amount of radiation as it emits. This equilibrium results in a steady temperature for the object.
radiative zone
radiative zone
G. W. Paltridge has written: 'Radiative processes in meteorology and climatology' -- subject(s): Atmospheric radiation, Radiative transfer
The radiative zone extends from the outer edge of the solar core to about 70% of the distance to the solar surface. It is approximately 200,000 kilometers thick.
by the radiative zone
Alistair F. Phillips has written: 'Temperature dependence of the radiative and non-radiative currents in visible and near infra-red semiconductor lasers'
Ngee-pong Chang has written: 'On radiative corrections to weak interactions' -- subject(s): Radiative corrections, Weak interactions (Nuclear physics)