Our Sun

How does energy move from the Sun's core to the Earth's surface?

Uses Hydrogen as a fuel source

Powered by nuclear fusion

Nuclear Fusion = two Hydrogen atoms combine to form a helium atom

When they collide, they produce energy in the form of radiation

Main-Sequence Star

4.6 billion years old (based on mass)

Estimated life span = 10 billion years

Product of something that produces energy

Transfers energy through waves

Waves can travel through matter, as well as through empty space

Core

Radiative Zone

Convection Zone

Photosphere

Chromosphere

Corona

Extremely hot and dense

Plasma gas (charged Hydrogen atoms)

Hydrogen atoms are moving fast and constantly colliding

Upon collision they form Helium atoms and release radiation energy

15,000,000 degrees Celsius

Photons (light waves) travel via radiative diffusion

Area between the Core and Convective zone

Between 2,000,000 - 7,000,000 degrees Celsius

Extends from 200,000km to surface

2,000,000 degrees Celsius

Radiation travels via convection currents

"Lava lamp"

the visible "surface" of the sun

6,000 degrees Celsius

Reddish gaseous layer

Part of Sun's outer-atmosphere

4,000 - 50,000 degrees Celsius

Aura of plasma

Outer-layer of Sun's atmosphere

10 million times less dense than Sun's surface

Hot, electric, magnetic, gas is released from the sun into space

Solar winds

Sun spots

Solar flares

Coronal Mass Ejections