Discover How We Came to Know the Cosmos

Chapter 12. Red Giants and White Dwarfs

18th December 2017 by Dr Helen Klus

12.1 Red giants

When the Sun runs out of hydrogen to fuse in its core, it’ll no longer produce enough nuclear energy to counterbalance the force of gravity (as discussed in Chapter 11), and so it will contract slightly. This will cause it to increase in temperature, and allow hydrogen fusion to begin in the shell around the helium core.

Fusion creates extra radiation pressure, and this will cause the Sun to expand. The outer layers of hydrogen will decrease in temperature, which will make them redder, and the Sun will then be a red giant. All main sequence stars that are about 1/5 to 10 times the mass of the Sun will become red giants.[1]

Diagram showing the evolution of a Sun-like star.

Figure 12.1
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Diagram showing the evolution of a Sun-like star, from protostar to red giant. After this, the core will become a white dwarf, while the outer layers will form a planetary nebula.

Diagram showing that the final fate of stars depends on their mass.

Figure 12.2
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The evolution of stars depends on their mass, with the most massive stars becoming black holes.

The helium core of a red giant is so dense that it becomes degenerate. This means that it’s as dense as the Pauli exclusion principle (discussed in Book II) allows, and it won’t be able to change in size as it changes in temperature.

It cannot expand and cool when it’s heated by the hydrogen fusion in the shell around it, and eventually it gets so hot that the helium nuclei began to fuse into carbon via the triple alpha process. The carbon can then fuse with helium nuclei to become oxygen and neon.

In stars less than about 2.5 times the mass of the Sun, this process is known as a ‘helium flash’.[2] This is because helium fusion occurs in a matter of minutes to hours. The energy released by the helium flash means that the star becomes so hot that it stops being degenerate, it can then expand and cool. These stars are sometimes called horizontal branch stars.

When all the helium has been fused into other elements, radiation pressure decreases, and the star contracts again under gravitation. Much higher temperatures are needed for carbon and oxygen fusion to begin, and so this only occurs in stars over about 10 times the mass of the Sun.

Stars less than about 10 times the mass of the Sun become asymptotic-giant branch stars - red giants with inert, degenerate carbon/oxygen cores, that are fusing helium in the shell around the core. This helium fusion causes the star to become unstable and the envelope is ejected as a planetary nebula.

If the remaining core is less than about 1.4 times the mass of the Sun, then it becomes a white dwarf. If it’s more than about 1.4 times the mass of the Sun, then it becomes a neutron star or black hole (discussed in Chapter 13).

Photograph of the Cat’s Eye Nebula.

Figure 12.3
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Planetary Nebula: the Cat’s Eye Nebula.

Photograph of the Ring Nebula.

Figure 12.4
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Planetary Nebula: the Ring Nebula.

The triple alpha process

Diagram of the triple alpha process.

Figure 12.5
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The triple alpha process.

Helium fuses into carbon via the triple alpha process. Here, two helium nuclei (made of two protons and two neutrons) collide to produce a gamma ray and a beryllium nucleus (made of four protons and four neutrons). This decays into a carbon nucleus (made of six protons and six neutrons), a helium nucleus, and a gamma ray.

If the carbon nucleus collides with another helium nucleus, it will produce an oxygen nucleus. Neon nuclei are formed if oxygen nuclei fuse with another helium nucleus.

12.2 White dwarfs

Over 97% of stars in the Galaxy will become white dwarfs.[3] White dwarfs are stars that have ceased nuclear fusion, but still emit light from stored thermal energy.

White dwarfs have a mass that is comparable to the mass of the Sun, but they are compacted to a size comparable to the size of the Earth. They have a very thin hydrogen and helium atmosphere, and a crust that is about 50 km thick. It’s thought that there’s a crystalline lattice of carbon and oxygen below this.[4]

Diagram showing that white dwarfs are typically not much larger than the Earth.

Figure 12.6
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White dwarfs are roughly the size of the Earth and the mass of the Sun.

Photograph of white dwarfs.

Figure 12.7
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White dwarfs, image from the Hubble Space Telescope.

Photograph showing X-rays during a supernova.

Figure 12.8
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The remnant of a type Ia supernova, the Tycho Supernova Remnant. The background is in optical light. Higher energy X-rays are shown in blue, and lower energy X-rays are shown in red. These come from expanding debris, shaped by tangled magnetic field lines.

If a white dwarf is part of a binary system - and at least half of all stars are in binaries because stars are formed close to each other[5] - it may acquire mass from its companion. This extra mass increases the white dwarfs’ temperature but, because it’s degenerate, it cannot expand and cool. It can get so hot that carbon and oxygen begin fusing extremely quickly, creating explosions on the surface. These types of binaries are known as cataclysmic variables (CVs) or, if matter is constantly fusing, super soft X-ray sources (SSXS or SSS). If enough matter is accumulated, then the white dwarf will explode in a type Ia supernova (also known as a thermal runaway supernova), and eject its companion into space.[6]

If a white dwarf is part of a binary system then the crust may be stripped away, exposing the core. This is what’s happened to PSR J1719-1438 b, which is known as a diamond planet (discussed in Chapter 28).

When a white dwarf stops producing light, it’s known as a black dwarf. White dwarfs are expected to keep radiating for well over 14 billion years, however, and so the universe is not yet old enough to contain any.

12.3 References

  1. Laughlin, G., Bodenheimer, P., Adams, F. C., The Astrophysical Journal 1997, 482, 420–432.

  2. Bappu, M. K. V., Sahade, J., Wolf-Rayet and High-Temperature Stars, Springer Science & Business Media, 2012.

  3. Fontaine, G., Brassard, P., Bergeron, P., Publications of the Astronomical Society of the Pacific 2001, 113, 409–435.

  4. NASA, White Dwarf Stars, NASA - Imagine the Universe!.

  5. NASA, NASA Telescope Finds Planets Thrive Around Stellar Twins, NASA, 2006.

  6. NASA, Cataclysmic Variables, NASA - Imagine the Universe!.

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How We Came to Know the Cosmos: Space & Time

I Pre 20th Century theories

1. Constellations

2. Latitude and Longitude

3. Models of the Universe

4. Force, Momentum, and Energy

5. Newton’s theory of Gravity

6. The Age of the Universe

II 20th Century discoveries

7. Einstein’s theory of Special Relativity

8. Einstein’s theory of General Relativity

9. The Origin of the Universe

10. Galaxies

11. Stars

12. Red Giants and White Dwarfs

13. Supergiants, Supernova, and Neutron Stars

14. Black Holes

III Missions to planets

15. The planet Mercury

16. The planet Venus

17. The planet Earth

18. The Earth’s Moon

19. The planet Mars

20. The Asteroid Belt

21. The planet Jupiter

22. The planet Saturn

23. The planet Uranus

24. The planet Neptune

IV Beyond the planets

25. Comets

26. The Kuiper Belt and the Oort Cloud

27. The Pioneer and Voyager Missions

28. Discovering Exoplanets

29. The Search for Alien Life in the Universe

30. Where are all the Aliens?

V List of symbols

31. List of symbols

32. Image Copyright