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Welcome to our Physics lesson on Energy Transmission from Core to Surface of the Sun, this is the third lesson of our suite of physics lessons covering the topic of Sun and Planetary Motion, you can find links to the other lessons within this tutorial and access additional physics learning resources below this lesson.
The gamma photons produced in the Sun's core shift towards the surface of the Sun. Since temperatures are very high and matter is very compressed, the photons experience frequent collisions with matter particles. As a result, they are absorbed and re-emitted multiple times from solar matter causing them to lose energy. This random process produces a kind of Brownian motion, i.e. photons travel a long way until they get into the surface of the Sun. When this finally occurs, the photon's energy (and frequency) has decreased to the visible light level.
Another method of solar energy transmission is through convection, i.e. through gas currents. More specifically, the hot gas layers move from the core to the surface and cool down as a result, at the same time colder layers shift towards the inside and heat up.
You have reached the end of Physics lesson 22.2.3 Energy Transmission from Core to Surface of the Sun. There are 10 lessons in this physics tutorial covering Sun and Planetary Motion, you can access all the lessons from this tutorial below.
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