1. Stellar Evolution Chapters 16, 17 & 18

2. Stage 1: Protostars Protostars form in cold, dark nebulae. Interstellar gas and dust are the raw materials from which stars form.

3. Example of a star forming nebula Star Cluster N81

4. Gas condenses due to gravity, temperature increases. Gives off heat (infrared, but no light) Planets may form.

5. Growth of a Protostar They continue to accrete matter until temperature and pressure in core are high enough for fusion.

6. Gravity versus Pressure

7. Stage 2: Main Sequence It takes small red stars over 50,000,000 years to reach stage 2. Large blue stars take only 60,000 years to reach stage 2. Nuclear fusion begins when hydrogen starts to burn.

8. These stars generate energy by hydrogen fusion. 4 Hydrogen molecules smash together to form Helium and energy. Star begins to shine. Main Sequence Stars

9. Red Dwarfs Sun Class Blue Giants The type of Main Sequence star depends on initial mass. Bigger = Higher Temperature = bluer color. 20,000 K + 3,000 K

11. Lower Limit for stars Brown dwarfs, not massive enough to start fusion M<0.08M Sun

12. Upper limit for stars Very massive stars are give off so much energy the pressure of photons drives their matter into space Observations show the limit is 100M Sun

13. Stage 3: Red Giant Hydrogen fuel is running out. Core shrinks, begins helium fusion. Radiation pressure pushes atmosphere out and it expands.

14. What’s happening: As the core contracts, it gets hotter, heating the layer of gas around it. Hydrogen fusion starts in this shell causing the atmosphere to expand. As it expands, it cools and becomes redder.

15. During stage 3, dredge ups occur when the star has a small mass.

16. Stage 4: Low Mass Star - White Dwarf White dwarfs, are the carbon and oxygen cores of dead stars. WD are about the size of earth. The more massive a WD is, the smaller it is in size.

17. Electron degeneracy pressure supports them against gravity. Eventually WD cool down, they end up cold, dense and dark – a black dwarf. WDs are surrounded by planetary nebula, the remains of the star’s atmosphere.

18. Nova Nova- Occurs in binary system, white dwarf + other aging star. Gases from companion fall on white dwarf surface. Outer layer of WD burns hydrogen. Can happen repeatedly.

19. Stage 3 High Mass Stars- Red Supergiant A high mass star, can have a diameter of 778 Million km, which is almost the size of Jupiter’s orbit.

20. Once helium in the core is consumed. The core contracts & heats up. A new element begins to burn. The surrounding layers heat, they also undergo fusion. The last stage is when iron is formed in the core!

21. High Mass Star Stage 4: Supernova When the most massive stars run out of fuel gravity quickly crushes the core. The atmosphere is ripped apart by shock waves in a cataclysmic explosion.

22. A supernova explosion can create a neutron stars or black holes.

23. Stage 5: Neutron Stars Formed by core collapse of very massive star. This star is so heavy due to protons and electrons being converted to neutrons in a very small space. Neutron degeneracy pressure of neutrons supports star against gravity.

24. Most Massive Stars Stage 5: Black Hole Collapsed core of most massive stars. Infinitely small & dense. Its gravity stops even light. The spherical surface is known as the event horizon. Astronomers believe black holes exist because they bend the fabric of space.

25. If we can’t see black holes, how do we know they are there?

26. Summary of Stages