1. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 1 Announcements: -Public Viewing THIS Friday Evergreen Valley College http://www.evc.edu 7PM-10:30 check website for weather information maps available online Pick up copy of handout: required for credit!! Homework #9 due today Exam #3: May 3 (Chp 12, 13)

2. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 2 Chapter 13

3. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 3 Introduction Where do stars come from? Giant Molecular Clouds Bok Globules Interstellar Medium (ISM) Protostars Pre-Main Sequence Stars How do they age (evolve) What is their fate?

4. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 4 Bi-polar jets Herbig-Haro objects (HH objects) Brown Dwarfs Contraction timescales depend on mass Hydrostatic Equilibrium

5. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 5 A Star’s Mass Determines its Core Temperature Hydrostatic Equilibrium: gas pressure balances gravity higher gravity, higher internal pressure, higher internal temperature!

6. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 6 Main Sequence Lifetimes High-mass stars have more fuel available (larger gas tanks) However, they burn their fuel more quickly (always speeding) In the end, they run out of gas sooner.  In solar units

7. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 7 A B0 Main Sequence star is 17.5 times more massive than the Sun and 30,000 times more luminous. Such a star will spend approximately _____ years on the Main Sequence. a) 30,000 b) 6 million c) 1,700 d) 1.7x10 13 e) 17.5x10 13

8. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 8 High mass stars are the first to reach the Main Sequence and the first to leave!

9. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 9 What happens to the star when it runs out of hydrogen? No hydrostatic equilibrium! Core begins to collapse. Core temperatures rise. Hydrogen shell burning.

10. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 10 What happens to the star when it runs out of hydrogen? Core contracts and heats up. Outer layers expand Shell burning begins. Outer layers expand a lot! Red Giant

11. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 11 What happens to the star when it runs out of hydrogen? Radius increases Surface temperature decreases Star moves toward upper right corner of HR Diagram Red Giant!!

12. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 12 What happens to the star when it runs out of hydrogen? Eventually, core temperatures are high enough to begin fusion of Helium nuclei into Carbon. (T=100 million K) 4 He + 4 He + 4 He  12 C Alpha particles Triple Alpha Process

13. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 13 Sun becomes a Red Giant

14. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 14 High-mass stars burn their fuel more quickly!

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16. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 16 A B C Youngest to oldest: a) B, C, A b) A, C, B c) C, A, B d) C, B, A

17. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 17 The Demise of a Sun-like Star: No hydrostatic equilibrium! Core begins to collapse. Core temperatures rise. Hydrogen and Helium shell burning. Second “red giant” ascent. And then……

18. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 18 At the end of its life, a star like the Sun will shed its outer layers.

19. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 19 Planetary Nebulae: The Ring Nebula Typical size: 0.25 ly Typical velocity of expanding material: 20 km/s

20. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 20 Typical Shape: conical along rotation axis

21. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 21 Catseye Nebula

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23. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 23 Which of the following sequences correctly describes the evolution of the Sun from young to old? a) white dwarf, red giant, main sequence, protostar b) red giant, main-sequence, white dwarf, protostar c) protostar, red giant, main sequence, white dwarf d) protostar, main sequence, white dwarf, red giant e) protostar, main sequence, red giant, white dwarf

24. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 24 Old Age of Massive Stars: Massive stars do not stop with helium fusion – a variety of Massive stars do not stop with helium fusion – a variety of nuclear reactions creates heavier elements. nuclear reactions creates heavier elements. Formation of heavy elements by nuclear burning processes is Formation of heavy elements by nuclear burning processes is called nucleosynthesis. called nucleosynthesis. Proton-proton chain Triple-alpha process (helium to carbon) 4 He + 12 C = 16 O +  where  is a gamma ray photon 16 O + 16 O = 28 Si + 4 He

25. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 25 Old Age of Massive Stars: As the temperature of the core increases, heavier elements are As the temperature of the core increases, heavier elements are fused forming concentric layers of elements. fused forming concentric layers of elements. Iron is the heaviest element fused (at about 1 billion K) - larger Iron is the heaviest element fused (at about 1 billion K) - larger elements will not release energy upon being fused. elements will not release energy upon being fused.  CORE COLLAPSE!

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27. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 27 NGC 3603: 2 million years old

28. Copyright © The McGraw-Hill Companies, Inc. Permission required for reproduction or display 28 Stars like the Sun probably do not form iron cores during their evolution because a) all of the iron is ejected when they become planetary nebulae b) their cores never get hot enough for them to make iron by nucleosynthesis c) the iron they make by nucleosynthesis is all fused into carbon d) their strong magnetic fields keep their iron in the atmosphere e) none of the above