The Evolution of Stars

1. The Evolution of Stars

2. Stellar Birth and Reaching the Main Sequence After birth, newborn stars are very large, so they are very bright. Gravity causes them to contract, and they become fainter because of their smaller sizes. After contracting for millions of years, stars eventually become hot enough to fuse hydrogen, which halts their contraction. They now maintain a stable size and luminosity until they run out of hydrogen fuel. This is the main sequence. contracting newborn stars contracting contracting contracting Main sequence (hydrogen fusion here) brown dwarfs

3. The Main Sequence Lifetimes of Stars All stars spend most of their lives on the main sequence, but the length of time on the main sequence (i.e., the time spent fusing hydrogen) depends a lot on a star’s mass. A star with a higher mass has a core with:  higher gravity  higher pressure  higher temperature  fuses hydrogen faster Although more massive stars have more hydrogen fuel, they consume that fuel at a much higher rate than less massive stars. As a result, more massive stars exhaust their fuel much faster and have shorter main sequence lifetimes. The lifetimes for the most massive stars are only a few million years while the least massive stars fuse hydrogen for trillions of years. A star with the mass of the Sun fuses hydrogen for 10 billion years.

4. The Main Sequence Lifetimes of Stars few million years 10 billion years >1 trillion years Sun

5. The Main Sequence Lifetimes of Stars

6. Evolution Beyond the Main Sequence After a stars exhaust its hydrogen fuel, its fate is determined by its mass at birth. Low-mass stars (<8 M) end their lives as white dwarfs High-mass stars (>8 M ) undergo supernova explosions, leaving behind neutron stars or black holes Main sequence (hydrogen fusion here)

7. Central Temperature H 100,000 K Gravity pulls the star inward Gas pressure resists gravity The protostar collapses and gets smaller, causing the pressure and temperature to increase in the center.

8. Central Temperature H 1,000,000 K Gravity pulls the star inward Gas pressure resists gravity The protostar collapses and gets smaller, causing the pressure and temperature to increase in the center.

9. Central Temperature 10,000,000 K H The star’s center eventually becomes hot enough to ignite hydrogen fusion, which stops its collapse. The star is now on the Main Sequence.

10. Central Temperature 10,000,000 K H Lots of hydrogen out here, but it’s not hot enough to fuse He Eventually, fusion converts all of the hydrogen in the core to helium.

11. Central Temperature 30,000,000 K H He Without fusion to hold it up, the core of the star contracts because of gravity.

12. Central Temperature 50,000,000 K H He As it contracts, the core grows hotter, and a shell of hydrogen surrounding the core becomes hot enough to fuse.

13. Central Temperature 50,000,000 K H He The radiation from the shell of fusing hydrogen is so intense that it pushes on the outer layers of the star, causing the star to expand to a huge diameter. The star is now a red giant.

14. Red Giants expanding red giants expanding Because the surface of the star has expanded so far from the core, it becomes cooler, and hence redder. This is why red giants are red. Although cooler objects produce less light (for a given size), the larger diameter and surface area more than make up for this, and the star’s luminosity increases a great deal. expanding expanding Main sequence (hydrogen fusion here)

15. Central Temperature Expanded view of core; outer layers of star not shown H fusion 100,000,000 K He fusion 3 4He 12C then 12C + 4He 16O The contracting core eventually becomes hot enough to begin fusing helium. This new energy source halts the core’s collapse.

16. Central Temperature H fusion 100,000,000 K He fusion C and O Eventually, the He in the core is converted to C and O. The core resumes its contraction once again.

17. Central Temperature H fusion 200,000,000 K He fusion C and O

18. Central Temperature 300,000,000 K H fusion He fusion C and O If the core’s mass is <1.4 M, the contraction is halted when the core becomes so dense that the atoms can’t be packed more tightly. This resistance to further compression is called electron degeneracy.

19. white dwarf C and O planetary nebula The radiation from the core (which is still very hot and bright) pushes the outer layers of the red giant into space, forming a planetary nebula. After this nebula dissipates, only the core of the star remains. This is called a white dwarf. It will cool and fade very slowly forever.

20. A star with an initial mass of <8 M will produce a core that has a mass of <1.4 M. In other words, stars with masses <8 M end their lives as white dwarfs. So the Sun will one day become a white dwarf. eventual C/O core = 1.4 M initial mass of entire star = 8 M

21. Evolution of Low-mass Stars after the Main Sequence planetary nebulae red giants white dwarfs

27. Planetary Nebulae Helix Nebula Ring Nebula When astronomers first looked at planetary nebulae through telescopes, the colors reminded them of planets like Mars, which is how they were given their name. We now know they they are unrelated to planets, but the term is still used.

28. Planetary Nebulae Eskimo Nebula NGC 6751

29. Planetary Nebulae Hourglass Nebula M2-9

31. White Dwarfs • White dwarfs have diameters that are similar to that of the Earth, but they can have as much mass as the Sun, so they are very, very dense. • All white dwarfs have masses <1.4 M because if the mass was higher, gravity would be strong enough to overcome electron degeneracy, and it would collapse and become an even denser and more compact object called a neutron star.

32. Central Temperature >1,000,000,000 K H fusion He fusion C,O fusion If the core’s mass is >1.4 M (i.e., initial star mass >8 M), gravity is strong enough to overcome electron degeneracy, and the core contracts to the point that it’s hot enough for carbon fusion.

33. The Death of a High Mass Star The fusion of C and O halts the collapse of the core for a short time. But after the C and O is fully converted to a heavier element (Mg), contraction resumes.

34. The Death of a High Mass Star Over time, progressively heavier elements are fused within the core of the star and in shells surrounding it.

35. The Death of a High Mass Star When the star’s core fuses into iron, it resumes its collapse once again. The core eventually becomes hot enough to ignite the fusion of iron. However, the fusion of iron spells disaster for the star…

36. The Death of a High Mass Star The products of iron fusion weigh more than the initial iron nucleus. According to E = m c2, this means that iron fusion does not make energy, it absorbs energy. Because it absorbs energy, iron fusion causes the temperature to decrease, and hence the gas pressure decreases, causing the collapse of the core to accelerate rather than halt. The core implodes in instant, forming a neutron star or a black hole at the center. Some of the imploding core rebounds off of the matter at the center of the core, sending a shock wave outward that blows the star apart. This is a Type II supernova explosion.

37. Type II Supernova Explosion

38. Type II Supernova Explosion For about a month, a supernova will shine brighter than an entire galaxy of 100 billion stars.

39. Evolution of High-mass Stars after the Main Sequence neutron stars red giants supernovae black holes After the red giant stage, a high-mass star (>8 M) undergoes a Type II supernova explosion, leaving behind a neutron star or a black hole. Neither of these objects is plotted on an H-R diagram because they produce little or no light.

40. The Origin of Heavy Elements Only the lightest 3 elements were present when the universe was born.

41. All heavier elements were made in the centers of stars, either during fusion or during Type II supernova explosions. All elements heavier than iron are created in supernovae.

42. Supernova Remnants

43. Galactic Supernovae In the Milky Way, a Type II supernova occurs once every couple hundred years. The last few were: SN 1006 (1006 A.D.) Crab Supernova (1054 A.D.) Tycho’s Supernova (1572 A.D.) Kepler’s Supernova (1604 A.D.) Casseopia A (1680 A.D.?)

45. Neutron Stars A Type II supernova explosion leaves behind either a neutron star or a black hole. In a neutron star, the electrons have been crushed into the atomic nuclei, so the star is one gigantic atomic nucleus made up only of neutrons.

46. Neutron Stars Neutron stars have masses that are similar to that of the Sun, but they are extremely small – only a few miles across. Because neutron stars are so small, they spin very rapidly, due to conservation of angular momentum. Neutron stars rotate once in only a second or less.

47. Pulsars Neutron stars are extremely small, so, according to L= R2T4, their luminosities are tiny. However, they can beam light out from their magnetic poles. As the neutron star rotates, this beam of light can sweep across the Earth periodically like a searchlight. This variety of neutron star is called a pulsar.

48. What Supports a Star Against Gravity? What if a neutron star is greater than ~ 3 M? Gravity is strong enough to crush the neutrons into each other, and nothing can hold up the star. This is a Black Hole.