1 / 45

The origin of the (lighter) elements The Late Stages of Stellar Evolution

The origin of the (lighter) elements The Late Stages of Stellar Evolution. Supernova of 1604 (Kepler’s). High-Mass Stars. > 8 M Sun. Intermediate-Mass Stars. Low-Mass Stars. < 2 M Sun. Brown Dwarfs. Broken thermostat. ‘Helium flash’.

berndt
Download Presentation

The origin of the (lighter) elements The Late Stages of Stellar Evolution

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  1. The origin of the (lighter) elementsThe Late Stages of Stellar Evolution Supernova of 1604 (Kepler’s)

  2. High-Mass Stars > 8 MSun Intermediate-Mass Stars Low-Mass Stars < 2 MSun Brown Dwarfs

  3. Broken thermostat

  4. ‘Helium flash’ Core of helium is supported by electron degeneracy pressure

  5. Helium burning stars are temporarily stable.

  6. After the Helium Flash

  7. After He fusion stops in the core… Variable stars:RR Lyrae Cepheids

  8. The Death of a Low-Mass Star: Planetary Nebula Remnants of stars with ~ 1 – a few Msun Radii: R ~ 0.2 - 3 light years Expanding at ~10 – 20 km/s ( Doppler shifts)  Last < 10,000 years Have nothing to do with planets! The Helix Nebula

  9. The Formation of Planetary Nebulae Two-stage process: Slow wind from a red giant blows away cool, outer layers of the star The Ring Nebula in Lyra Fast wind from hot, inner layers of the star overtakes the slow wind and heats it => Planetary Nebula

  10. The Cat Eye Nebula: • Approx 3000 LY away • Central star T = 80,000 K • Spectral class O • Mass ~ 1 Msun • Radius ~ 0.65 Rsun

  11. The Cat Eye

  12. White Dwarfs are supported by electron degeneracy pressure • in a low-mass star, Fusion stops after He -->C and O • Just cools off and fizzles out Siruis and its white dwraf companion, Sirius B

  13. Summary: Evolution of a Sun-Like Star

  14. Earth’s Fate • Sun’s luminosity will rise to 1,000 times its current level—too hot for life on Earth

  15. Earth’s Fate • Sun’s radius will grow to near current radius of Earth’s orbit

  16. High mass stars : CNO Cycle • H fusion is faster because C, N and O act as catalysts • Same net result: 4 H become 1 He. • No total gain or loss of C, N, O

  17. Life Stages of High-Mass Stars • high-mass stars are similar to low-mass stars: • Hydrogen core fusion (main sequence) • Hydrogen shell burning (supergiant) • Helium core fusion (subgiant) • They are also different.. • H-->He via CNO cycle not p-p chain • Core much hotter • fuse C, O into heavier elements • He core is not degenerate • no He flash! • Lose a lot of mass

  18. High-mass stars make the elements necessary for life!

  19. Big Bang made 90% H, 10% He – stars make everything else

  20. Helium fusion can make only carbon in low-mass stars

  21. Helium Capture occurs only in high-mass stars • High core temperatures allow helium to fuse with heavier elements

  22. Helium capture builds C into O, Ne, Mg, … Total # of P+N = Multiples of 4! Why?

  23. Evidence for helium capture: Higher abundances of elements with even numbers of protons

  24. Advanced Nuclear Burning • Core temperatures in stars with >8MSun allow fusion of elements up to iron

  25. Si, S, Ca, Fe, etc. can only be made in high-mass stars

  26. Multiple Shell Burning • Advanced nuclear burning proceeds in a series of nested shells

  27. Fusion releases energy only when the mass of the products < mass of the reactants • Iron is “ash” of fusion: nuclear reactions involving iron do not release energy • Iron-56 has lowest mass per nuclear particle • Highest “binding energy” of all the elements

  28. How does a high-mass star die? Iron builds up in core until degeneracy pressure can no longer resist gravity

  29. Supernova Explosion • Core degeneracy pressure cannot support degenerate core of > 1.4 Msun • electrons forced into nucleus, combine with protons • making neutrons, neutrinos and LOTS of energy!

  30. Collapse only takes very short amount of time (~seconds) Supernova!

  31. Energy and neutrons released in supernova explosion cause elements heavier than iron to form, including Au and U

  32. Neutron Stars & Supernova Remnants • Energy released by collapse of core drives outer layers into space • The Crab Nebula is the remnant of the supernova seen in A.D. 1054

  33. Supernova 1987A • The first visible supernova in 400 years

More Related