Age of M13: 14 billion years. Mass of stars leaving the main-sequence ~0.8 solar masses

2. Age of M13: 14 billion years. Mass of stars leaving the main-sequence ~0.8 solar masses Helium core-burning stars Giants Sub-giants Main Sequence

3. Here is a way to think about it. Outside of star Plenty of hydrogen Shrinking core Where core use to be. And where conditions were right for fusion.

4. Result… • Because the core is shrinking there is hydrogen that is introduced into the area around the core where temperatures and pressures are high enough for hydrogen fusion to take place. • Hydrogen begins to fuse into helium, in a shell around the shrinking helium core. • Now there are two energy sources in the star.

5. Two energy sources. • Gravitational potential energy is being used to make radiant energy in the core. • The shell around the core is producing energy from the fusion of hydrogen. • The result of all this energy is that the outer envelope of the star expands enormously. The star becomes a red giant. (luminosity class III)

6. Age of M13: 14 billion years. Mass of stars leaving the main-sequence ~0.8 solar masses Helium core-burning stars Giants Sub-giants Main Sequence

7. Helium core burning • The core contraction and hydrogen shell burning until at last the temperature is high enough in the core to begin helium fusion. This is around 100 million degrees. • When this happens the star is fusing Helium into Carbon in its core, and still is fusing Hydrogen into Helium is a shell around the core.

8. The triple alpha process

9. Core and shell burning produces more energy than the star produced on the main sequence so the He-core burning stars are more luminous than when they were main-sequence stars. Helium core-burning stars Giants Sub-giants Main Sequence

10. Helium gone in the core • Helium fusion rate is much faster than the Hydrogen fusion rate was. Within a few hundred million years the supply is gone in the core. • The core once again shrinks, releasing gravitational potential energy. • The material in a shell closest to the core begins to fuse helium into carbon, in bursts, as the temperature increases. • Above this shell, hydrogen is being converted into helium.

11. Here is a way to think about it. Outside of star Helium shell burning Plenty of hydrogen Shrinking core Hydrogen shell burning

12. Three energy sources. • At this point there are three sources of energy in the star, the shrinking carbon core, and two shells. • The star rapidly expands and heads back up to the giant stage. This is called the asymptotic giant branch, because it asymptotically approaches the red giant branch.

14. Asymptotic Giant branch phase • During this phase the helium core burning is not stable. It rapidly turns on and off in bursts. Small explosions. • The results of these explosions is to eject shocks into the outer envelope of the star. Material in the envelope is lifted off the star, over and over again. • When the carbon core can no longer contract, everything stops.

15. The lost envelope becomes an expanding planetary nebula. • The exposed carbon core is a white dwarf star.

16. Planetary nebula & White Dwarf White Dwarf star

17. Summary of evolution of lower mass stars • Star is on main-sequence – Core converting hydrogen into helium. • Star is a Sub-giant -- Core is contracting releasing gravitational potential energy • Star is a Giant (III) – Core is contracting releasing gravitational potential energy and hydrogen into helium in a shell around the core. • Helium core burning phase – Star is converting helium into carbon in the core and hydrogen into helium in a shell. • Asymptotic Giant branch phase – Core is contracting releasing potential energy, Helium into Carbon in a shell, and hydrogen into helium is a shell around Helium shell.

18. Notice a pattern • Whenever a star has an inert core that is shrinking, the star is moving up the giant branch. The star grows in radius • Whenever there is nuclear fusion in the core the star shrinks back down. Smaller radius. • This will be important in high mass stars.

19. Inert core Core fusing elements

20. Low mass stars cannot fuse Carbon • Core temperature is too low to fuse Carbon into other elements. • The core shrinks until all the free electrons are trapped in spaces between the Carbon nuclei. They set up energy levels and the core acts like a giant atom. Core cannot shrink any more. • The core is similar in size to the radius of the Earth, but has a mass of as high as 1.4 times the Sun’s mass. • From here on the core will just slowly cool off. Like a hot piece of metal, slowly cools down.

21. Planetary Nebula • During the Helium shell burning phase, there are helium flashes occurring. The helium in the shell doesn’t “burn” at a constant rate. It burns in spurts. Each time helium shell burning turns on, there is an eruption. • The result is the outer envelope of the star gets shocked, over and over. The outer shell is lifted off in layers. • The result is a planetary nebula. The exposed Carbon core is a white dwarf.

22. The Ring nebula – M57

23. Cat’s Eye Nebula

24. M57 through a small telescope

25. Boomerang Nebula

26. Butterfly Nebula – Central White Dwarf has T = 250,000 K.

27. Cat’s Eye in optical and X-ray light

28. Eskimo Nebula

29. NGC 2440 – Central White Dwarf has T = 200,000 K

30. Ring Nebula – Multiple mass ejections.

31. The planetary nebula phase is short lived. • The radius of a typical planetary nebula is about 1 light year. • The gas is glowing, so we see an emission nebula. • Typical elements in at planetary nebula are hydrogen, helium, carbon, oxygen and nitrogen. Also some neon present.

32. Spectrum of Ring nebula

34. Sirius – The Dog Star

35. Sirius is a binary star Sirius A Sirius B

37. Which star is older in this binary system 30 • Sirius B because it is already a white dwarf • Sirius A because it is more luminous • They are in a binary system, they must be the same age 0 30

38. Which star was originally the most massive? 30 • Sirius B because it is a white dwarf • Sirius A because it is more luminous • They formed at the same time so they must have the same mass 0 30

39. Globular cluster M 4

40. The stars with masses higher than about 0.8 solar masses have died. • There should be a lot of white dwarfs in the a globular star cluster.

41. White Dwarfs in M 4

42. White dwarfs are just the leftover core of the star. It is not producing energy. It is simply cooling off. • As a WD cools it becomes less luminous because the temperature is decreasing. • The cooling follows a very simple cooling relation that depends primarily on time. The older the white dwarf, the cooler it is. • There is a cutoff in the WD temperature. No WD are found that are cooler than the cut off.

43. Cooling Cut-off

44. Why is there a cut-off in the white dwarf population? 30 • Cooler WD are impossible to detect • At a certain temperature, WD explode • The universe isn’t old enough to have cooler white dwarfs • WD come into temperature equilibrium with the universe and remain that temperature 0 60

45. Age of the universe using WD cooling • To date hundreds of thousands of White Dwarfs have been observed. • There is a temperature cut-off beyond which no white dwarfs are found. • This is because there hasn’t been enough time since the start of the universe for WD to cool any further. • The age of the universe computed from WD cutoff is about 12 billion years.

46. The Death of High Mass Stars

47. When a high mass star runs out of hydrogen in its core, the core begins to shrink. The outside of the star expands and the star moves right on the H-R diagram. • The temperature is cooling and the radius is growing, but the luminosity is virtually constant. • Since L = σT4(4πR2); T4 must be changing at the same rate as R2 • The star becomes a supergiant (luminosity class I star)

48. The Death of High Mass Stars

49. As the star tracks to the right for the first time the inert helium core is contracting and hydrogen shell burning is occurring. • At the farthest right, helium core burning begins, converting helium into carbon. And still hydrogen shell burning. • The star begins to move to the left on the H-R diagram.

50. The Death of High Mass Stars