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Astronomy Picture of the Day

Astronomy Picture of the Day. Stellar Evolution Video. Review Question. The surface of the Sun, or the part of the Sun that we see, is called the _________ . A) core B) photosphere C) corona D) radiation zone. Review Question. The apparent brightness of a star depends on its:

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Astronomy Picture of the Day

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  1. Astronomy Picture of the Day Stellar Evolution Video

  2. Review Question • The surface of the Sun, or the part of the Sun that we see, is called the _________ . • A) core • B) photosphere • C) corona • D) radiation zone

  3. Review Question • The apparent brightness of a star depends on its: • A) mass and temperature • B) size and velocity • C) age and temperature • D) luminosity and distance from Earth

  4. Review Question • Sunspots are associated with “loops” created in the Sun's magnetic field as a result of _____ . • A) convection • B) flares • C) differential rotation • D) the solar wind

  5. Question When a star runs out of hydrogen, what happens next?

  6. Evolution of a Low-Mass Star (< 8 Msun , focus on 1 Msun case) - Helium ash collects in core. • - Too cool for He burning. Why? - Core contracts. Heats up. H burning shell - Higher temp. => Brighter! Star expands! - "Red Giant". Diameter ~ 1 AU! - Does fusion rate at this stage increase or decrease? Why? Red Giant

  7. Evolution of a Low-Mass Star (< 8 Msun , focus on 1 Msun case) - Helium ash collects in core. • - Too cool for He burning. Larger electric repulsion. - Core contracts. Heats up. H burning shell - Higher temp. => Brighter! Star expands! - "Red Giant". Diameter ~ 1 AU! - Rate increases. Phase lasts ~ 1 billion years Red Giant

  8. Creation of Heavier Elements - Core shrinks and heats up to 108 K, => Helium fuses into Carbon. - All He -> C. - Core shrinks and heats up. - Onion-like structure • Each phase shorter than the last. Red Supergiant

  9. Death of a Low Mass Star • What factor(s) eventually determine when this process stops?

  10. "Planetary Nebulae" • - Low mass star (< 8 Msun) cannot achieve 600 Million K temp. needed for Carbon fusion • -Contraction stopped by the Pauli exclusion principle: two objects cannot occupy the same space. - Star becomes unstable. Ejects outer layers. "Planetary Nebula" (Historical name, nothing to do with planets.) • - Carbon core called a “White Dwarf”

  11. Stellar Lifetimes • Is the lifetime of a high mass star shorter or longer than that of a lower mass star? Why?

  12. Evolution of Stars > 8 MSun Eventual state of > 8 MSun star Higher mass stars burn out faster and fuse heavier elements. Example: 20 MSun star lives "only" ~10 million years. Heaviest element made in core of any star is iron. Products of outer layers become fuel for inner layers

  13. Stellar Explosions Novae White dwarf in binary system WD steals mass from companion. Eventually, a burst of fusion. Brightens by 10'000's! Cycle may repeat every few decades => recurrent novae.

  14. Nova Cygni with Hubble May 1993 Jan 1994 1000 AU Is all of the accreted matter expelled into space during a nova?

  15. A Carbon-Detonation or “Type I” Supernova Despite novae, mass continues to build up on WD. At 1.4 MSun(the "Chandrasekhar limit"), gravity overwhelms the Pauli exclusion pressure supporting the WD => contraction and heating. Carbon fusion everywhere at once. Tremendous energy makes star explode. No core remnant.

  16. Death of a Very High-Mass Star M > 8 MSun Iron core at T ~ 1010 K radiation photodisintegrates iron nuclei into protons and neutrons. Core collapses in < 1 sec. Neutrons “rebound”. Shock ejects outer layers => Core-collapse or Type II Supernova Ejection speeds 1000's to 10,000's of km/sec! Remnant is a “neutron star” or “black hole”. (Supernova Demo)

  17. Supernova 1987A in the Large Magellanic Cloud

  18. In 1000 years, the exploded debris might look something like this: Crab Nebula: debris from a stellar explosion observed in 1054 AD. 2 pc Or in 10,000 years: Vela Nebula: debris from a stellar explosion in about 9000 BC. 50 pc

  19. Remember, carbon-detonation (Type I) and core-collapse (Type II) supernovae have very different origins

  20. Testing our Theories • How can we test our theories of stellar evolution when the lifetimes of stars are so long?

  21. Star Clusters Two kinds: 1) Open Clusters -Example: The Pleiades -10's to 100's of stars -Young (10's to 100's of millions of years)

  22. 2) Globular Clusters - few x 10 5 or 10 6 stars - Billions of years old Why are star clusters useful for stellar evolution studies?

  23. Clusters are useful for stellar evolution studies because all of the stars: 1) formed at about same time 2) are at about the same distance 3) have same chemical composition The ONLY variable property among stars in a cluster is mass!

  24. Making the Heaviest Elements • Since iron is the heaviest element that can be made by stellar fusion, where do the heavier elements come from?

  25. Making the Elements H and some He were made in Big Bang. Rest made in stars, and distributed by supernovae. Heaviest elements made in supernovae. Solar System formed from such "enriched" gas 4.6 billion years ago.

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