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Astro 201: Oct. 5, 2010

Astro 201: Oct. 5, 2010. Today : The Evolution of the Sun The Evolution of Massive Stars Origin of the Elements White Dwarfs, Neutron Stars, Black Holes. Illustrations from Prof. Terry Herter's web site and Prof. Richard Pogge's web site. 1. Protostar Phase (50 million years)

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Astro 201: Oct. 5, 2010

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  1. Astro 201: Oct. 5, 2010 • Today: • The Evolution of the Sun • The Evolution of Massive Stars • Origin of the Elements • White Dwarfs, Neutron Stars, Black Holes

  2. Illustrations from Prof. Terry Herter's web site and Prof. Richard Pogge's web site

  3. 1. Protostar Phase (50 million years) *Gas cloud undergoes Gravitational Contraction until fusion starts * The Sun took about 50 million years to reach the main sequence * During the collapse phase it was brighter and cooler than it is on the Main Sequence * The paths of protostars in the H-R diagram are called the Hayashi Tracks

  4. 2. MAIN SEQUENCE (10-11 billion years) The Sun reached the Main Sequence about 4.5 billion years ago At that time, it was fainter-- 0.70 x the luminosity of today's Sun it was a little smaller -- 0.897 x the radius of today's Sun it was a little cooler -- 5586 K

  5. On the Main Sequence, the Sun burns hydrogen to helium in the proton-proton process, and gets progressively hotter and brighter. Why? Because the pressure P=nkT where n= the number of atoms/volume, k=Boltzman's constant T=temperature. As 4 protons -> 1 helium, ndecreases so T increases in order to keep the pressure P high enough to counteract gravitational collapse

  6. 1.1 billion years from now, the Sun will be 10% brighter, and there will be a significant greenhouse effect on the Earth

  7. Independent of “Global Warming” We can measure the CO2 concentration in the atmosphere as a function of time, using bubbles trapped in ice layers in Antartica. (Last 50 years, direct measure). A steady increase in CO2 began in the mid-1800's, the result of increased burning of fossil fuels, associated with the growth of industry and urban populations. The increased CO2 causes an enhanced "greenhouse effect" and hence warming of the average temperature on Earth. Greenhouse Effect: Global warming from increased "greenhouse gas" production, particularly in the U.S. Greenhouse Gas: CO2, methane (from burning of coal, natural gas, and oil; livestock); nitrous oxide; hydroflurocarbons.

  8. 3.5 billion years from now, the Sun will be 40% brighter there will be a runaway greenhouse effect on the Earth: it will be like Venus. On the surface of Venus, atmospheric pressure = 90x Earth’s Average temperature = 737K or 900 F hot enough to melt lead

  9. End of the Main Sequence: 11 billion years after the Sun first reached the Main Sequence, the Sun turns into a RED GIANT STAR • Hydrogen is all converted into helium in the core • Helium core begins to collapse, since energy is no longer being produced to counteract the collapse by gravity • Hydrogen fusion to helium still occurs in a shell around the core • Star rearranges itself, eventually becoming a RED GIANT • Outer layers of the Sun expand, star becomes Larger, • surface temperature is cool (red) , very luminous • For the Sun, this process will take about 1 billion years

  10. At the top of the Red Giant Branch in the HR diagram, the Sun will be T=3107 K (M0 III) Luminosity=2350 x the luminosity of the current Sun Radius = 166 x Sun's current radius, engulfing Mercury During this time, the outer layers of the Sun escape in a stellar wind. The Sun will lose 28% of its mass.

  11. 4. The Helium Flash * When the core of the star gets hot enough, a new fusion process occurs: the TRIPLE ALPHA REACTION Alpha = alpha particle = helium nucleus * Triple Alpha: 3 helium --> 1 Carbon + energy * The fusion of helium into carbon causes an enormous production of energy in a few seconds. * Again, the star rearranges itself to be hotter and smaller – it becomes a so-called Horizontal branch star

  12. 5. The Horizontal Branch -- 100 Million yrs * The Sun burns Helium into carbon and oxygen in its core as a horizontal branch star for about 100 million years * It still is burning Hydrogen to helium in a shell around the core * At this point the Sun will be about R=18 x solar radius today, T=4450 K, L=110 x luminosity of the Sun today

  13. 6. The ASYMPTOTIC GIANT BRANCH * Eventually, the helium in the core is used up. The core is now Carbon and Oxygen and it begins to collapse. * There are shells of Helium burning and hydrogen burning still * Again, the Sun rearranges itself and becomes a RED GIANT Again * During this phase, what's left of the outer layers of the star are blowing off in a wind, until the Sun's mass is about 0.6 x what it is today * At the top of the Asymptotic Giant Branch, the star starts to pulsate, and is very unstable

  14. 7. Planetary Nebula Phase * Finally, the outer parts of the star are ejected. The core is extremely hot and dense, and lights up the ejected material in a "Planetary Nebula” * Short-lived phase The ejection of the PNE takes 100,000 years, but then the planetary shines only 10,000 years * Despite the short lifetime of Planetary Nebulae, the stars which end up as PNE are common: in the Milky Way today, there are about 10,000 planetaries * "Planetary" nebulae have nothing to do with planets: This is a misnomer from the days of small telescopes when the images were small, fuzzy blobs

  15. Images of Planetary Nebulae

  16. The Hourglass Nebula

  17. 8. White Dwarf Phase * The core collapses until ELECTRON DEGENERACY PRESSURE stops the gravitational collapse When the pressures are very high, electrons are squished together and resist further collapse Result of the Pauli Exclusion Principle * At this point, the star is a "White Dwarf" and slowly cools for the rest of time * Mass is about 0.5x solar mass today, but 200,000x more dense than Earth * The Sun will then be about the same size as the Earth * A teaspoon of electron degenerate material would weigh 5 tons

  18. White Dwarfs in Globular Cluster M4 (= 100 watt light bulb at distance of the Moon)

  19. SUMMARY: The LIFE STORY of the Sun 1. Collapsing Protostar: 50 million years 2. 1 Msun Main-Sequence Star: 11 billion years 3. Red Giant Branch Ascent: 1 billion years 4. Helium Flash: a few seconds 5. Horizontal Branch: 100 million years 6. Asymptotic Giant Branch Ascent: 20 million years 7. Thermal Pulse Phase: 400,000 yr 8. Envelope Ejection: < 100,000 yr 9. Planetary Nebula: 10,000 years 10. 0.5 Msun White Dwarf: …

  20. PROTOSTAR, MAIN SEQUENCE Phases of massive stars are similar to the Sun, just massive stars evolve faster and are much brighter A star with 20 solar masses spends 8 million years on the Main sequence, and 1 million years as a red giant, before blowing up as a supernova

  21. GIANT/SUPERGIANT phase stars with mass > 4 solar masses become so hot in their cores that HELIUM CAPTURE and the CNO cycle occur. CNO cycle:

  22. Final Result: Onion Skin Layers of heavy elements in CORE

  23. These stages are fast. For example, for a 25 Msun star: * Hydrogen fusion lasts 7 million years * Helium fusion lasts 500,000 years * Carbon fusion lasts 600 years * Neon fusion lasts 1 year * Oxygen fusion lasts 6 months * Silicon fusion lasts 1 day The star's core is now pure iron.

  24. . SUPERNOVA * The star hits the IRON wall: Iron is a very stable element, and cannot fuse to form heavier elements. * So when the core becomes IRON, fusion no longer produces enough energy to stop gravitational collapse * The core collapses, until neutron degeneracy pressure stops the collapse of the core. * The outer parts of the star hit the core and bounce off --> a supernova! * What's left is a NEUTRON STAR (if the mass is less than about 8 solar masses) or a BLACK HOLE

  25. Within a massive, evolved star the onion-layered shells of elements undergo fusion, forming an iron core And starts to collapse. The inner part of the core is compressed into neutrons (c), causing infalling material to bounce (d) and form an outward-propagating shock front (red). The shock starts to stall (e), but it is re-invigorated by a process that may include neutrino interaction. The surrounding material is blasted away (f), leaving only a degenerate remnant.

  26. Historic Supernovae: * Supernovae become extremely bright. * Supernovae in our Milky Way can become bright enough to see during the day. * Supernovae in distant galaxies are of intense interest now for cosmology * Famous Historic Supernova: 1054, recorded by Chinese and Native Americans, today is the Crab Supernova remnant 1006: Southern hemisphere supernova 1572: Tycho Brahe's supernova 1604: Kepler's supernova

  27. Since 1604, there have been no supernova explosions in the Milky Way -- we're overdue! In 1987, a supernova in the Large Magellanic Cloud, SN1987A Two neutrino experiments operating at that time detected neutrinos from the explosion Before and after picture

  28. IMAGES OF SUPERNOVA REMNANTS

  29. Crab Supernova Remnant, optical

  30. Crab Supernova Remnant in X-rays (Hot, million degree gas)

  31. Tycho’s Supernova Remnant

  32. Kepler’s Supernova Remnant

  33. Origin of the Elements * All the carbon, oxygen, etc on the Earth, (and in humans) was produced in the centers of stars. * Most carbon, oxygen comes from low-mass red giant winds * Most of the heavy elements come from supernovae * New stars form out of interstellar gas which has been enriched with elements by red giant winds, planetary nebulae and supernovae. * Older stars on the main sequence have relatively fewer atoms of iron than younger stars, since they were formed out of gas which had not been polluted by as many generations of stars * We've searched pretty hard, but have never found, pure hydrogen and helium stars.

  34. Radioactive Dating: How we knowThe age of the Earth & Solar Systemor: “Clocks in Rocks” • Some isotopes of atoms are unstable and undergo radioactive decay, splitting into 2 or more “daughter” atoms • Element: determined by # of protons • Isotope: determined by # of protons and # of neutrons • e.g. 87Sr, 90Sr and 86Sr are isotopes of Sr, or strontium, • all have 38 protons, but different number of neutrons

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