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Red Giant Stars

Drawing of a Red Giant
Credit: ESA/JAXA

When hydrogen fuel at the centre of a star is exhausted, nuclear reactions will start move outwards into its atmosphere and burn the hydrogen that’s in a shell surrounding the core. As a result, the outside of the star starts to expand and cool, turning much redder. Over time, the star will change into a red giant and grow to more than 400 times its original size.

As they expand, red giants engulf some of their close-orbiting planets. In the Sun's case, this will mean the fiery end of all the inner planets of our Solar System, which might also include the Earth; but don't worry, this won't happen for another 5,000,000,000 years.

While the atmosphere of the star grows, its core shrinks due to gravity. Temperatures and pressures in the middle increase until the conditions are right for nuclear fusion to start again, but this time using helium as a fuel, rather than hydrogen.

With the star being powered by helium, its outer layers return to normal for a while and it starts to shrink, get hotter and turn a little more blue. However, this stage only lasts for a million years or so, as the helium quickly runs out. When it does, the core shrinks again and this time the helium starts burn in a shell around the core and hydrogen may start burning in a shell around that! The outer layers of the star starts to grow, cool and turn red again as it enters its second red giant phase.

What happens next depends on the mass of the star. Small sun-like stars move into a planetary nebula phase, whilst stars greater than about 8 times the mass of the Sun are likely to end their days as a supernova.


Please note that over the weekend of the 26-28th May 2017 we will be switching over to our brand new website - during this time there may be periods where the site is difficult to access, and users will be unable to request observations from the telescope. Please bear with us during this time. All should be back up and running by the 29th May 2017.