1 / 11

Stellar Evolution

Stellar Evolution. Pg . 43. Basic Structure of Stars. Mass governs a star’s properties Energy is generated by nuclear fusion Stars that aren’t on main sequence of H-R either have fusion from other elements or don’t undergo fusion at all. Stellar Evolution and Life Cycles.

dalton
Download Presentation

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. Stellar Evolution Pg. 43

  2. Basic Structure of Stars • Mass governs a star’s properties • Energy is generated by nuclear fusion • Stars that aren’t on main sequence of H-R either have fusion from other elements or don’t undergo fusion at all

  3. Stellar Evolution and Life Cycles • Changes as it ages because fusion is continually making new elements • Eventually nuclear fuel runs out • All form from a nebula • As the cloud contracts, particle rotate into a disk with a protostar in the middle. • Eventually temp inside protostar is hot enough to start fusion • Hydrogen then begins converting to helium

  4. The Sun’s Life Cycle • Takes about 10 billion years for a star the size of the Sun to convert all the hydrogen into helium • After all H is converted, the core is He surrounded by H gas • The gas expands and cools producing a red giant (luminosity is increasing while temp is decreasing) • Gases escape and eventually helium is converted to carbon • The star shrinks back to normal size and now has a carbon core

  5. Cycle cont’d • Carbon never becomes hot enough to react • Outer layers expand again • Gas that leaves is called planetary nebula • The carbon core is left (Earth-size) • This creates a white dwarf

  6. White dwarfs • Stable because electrons inside the star resist being forced together • Doesn’t need heat to be maintained • Star that has less mass than the sun has a similar life cycle except the core never gets hot enough to fuse to carbon so it is a white dwarf with a He core • Smaller star has a longer lifetime because it doesn’t use up nuclear fuel as fast

  7. Life cycle of Massive stars • Starts higher on the main sequence and uses nuclear fuel very quickly • Undergoes more reactions so has many more elements in the core • Becomes a red giant several times (after each elemental stage) • After it expands, becomes a supergiant • Mass is eventually lost and it becomes a white dwarf

  8. Supernovae • Some stars don’t lose enough mass to become a white dwarf • Once reactions have created iron, the core collapses on itself • Protons and electrons merge to form neutrons • Neutrons can’t be squeezed together so collapsing stops and a neutron star is formed • Small but dense • Gas falling to the surface rebounds and explodes outward • Outer portion is blown off in an explosion called a supernova • Creates elements heavier than iron

  9. Black holes • Some stars are too massive to even form neutron stars • The core of such a star collapses forever compacting matter into smaller and smaller volumes • The small but dense object left is called a black hole because the gravity is so great that not even light can escape it

  10. Star Cycle • On page 44, I want you to create a diagram that illustrates the life cycle of a star. • Include a diagram for the following: • The evolution of a star • Life cycle of a star the size of our sun • Life cycle of a star bigger than our sun • When you are done, read the article on page 828 in the book, there will be a question from it on your next test

More Related