1. Everything you always wanted to know about stars…

2. The Spectra of Stars Inner, dense layers of a star produce a continuous (black body) spectrum. Cooler surface layers absorb light at specific frequencies.  Spectra of stars are absorption spectra.  Spectrum provides temperature, chemical composition

3. Spectral Classification of Stars (I) Temperature Different types of stars show different characteristic sets of absorption lines.

4. Oh Only BeBoy,Bad AAnAstronomers FineFForget Girl/GuyGradeGenerally KissKillsKnown Me Mnemonics Mnemonics to remember the spectral sequence:

5. Stellar spectra O B A F G K M Surface temperature

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7. We have learned how to determine a star’s surface temperature chemical composition Now we can determine its distance luminosity radius mass and how all the different types of stars make up the big family of stars.

8. Distances to Stars Trigonometric Parallax: Star appears slightly shifted from different positions of Earth on its orbit The farther away the star is (larger d), the smaller the parallax angle p. d = __ p 1 d in parsec (pc) p in arc seconds 1 pc = 3.26 LY

9. The Trigonometric Parallax Example: Nearest star,  Centauri, has a parallax of p = 0.76 arc seconds d = 1/p = 1.3 pc = 4.3 LY With ground-based telescopes, we can measure parallaxes p ≥ 0.02 arc sec => d ≤ 50 pc This method does not work for stars farther away than about 50 pc (nearly 200 light-years).

10. Intrinsic Brightness The more distant a light source is, the fainter it appears. The same amount of light falls onto a smaller area at distance 1 than at distance 2 => smaller apparent brightness. Area increases as square of distance => apparent brightness decreases as inverse of distance squared

11. Intrinsic Brightness / Flux and Luminosity The flux received from the light is proportional to its intrinsic brightness or luminosity (L) and inversely proportional to the square of the distance (d): F ~ L __ d2d2 Star A Star B Earth Both stars may appear equally bright, although star A is intrinsically much brighter than star B.

12. The Size (Radius) of a Star We already know: flux increases with surface temperature (~ T 4 ); hotter stars are brighter. But brightness also increases with size: A B Star B will be brighter than star A. Absolute brightness is proportional to radius squared, L ~ R 2. Quantitatively: L = 4  R 2  T 4 Surface area of the star Surface flux due to a blackbody spectrum

13. Example: Polaris has just about the same spectral type (and thus surface temperature) as our sun, but it is 10,000 times brighter than our sun. Thus, Polaris is 100 times larger than the sun. This causes its luminosity to be 100 2 = 10,000 times more than our sun’s.

14. The Hertzsprung Russell Diagram Most stars are found along the main sequence

15. The Hertzsprung-Russell Diagram (II) Stars spend most of their active life time on the Main Sequence. Same temperature, but much brighter than MS stars  Must be much larger  Giant Stars Same temp., but fainter → Dwarfs

16. Radii of Stars in the Hertzsprung-Russell Diagram 10,000 times the sun’s radius 100 times the sun’s radius As large as the sun 100 times smaller than the sun RigelBetelgeuse Sun Polaris

17. Luminosity Classes Ia Bright Supergiants Ib Supergiants II Bright Giants III Giants IV Subgiants V Main-Sequence Stars Ia Ib II III IV V

18. Examples: Our Sun: G2 star on the main sequence: G2V Polaris: G2 star with supergiant luminosity: G2Ib

19. Masses of Stars in the Hertzsprung- Russell Diagram Masses in units of solar masses Low masses High masses Mass The higher a star’s mass, the more luminous (brighter) it is: High-mass stars have much shorter lives than low-mass stars: Sun: ~ 10 billion yr. 10 M sun : ~ 30 million yr. 0.1 M sun : ~ 3 trillion yr. L ~ M 3.5 t life ~ M -2.5

20. Surveys of Stars Ideal situation: Determine properties of all stars within a certain volume. Problem: Fainter stars are hard to observe; we might be biased towards the more luminous stars.

22. A Census of the Stars Faint, red dwarfs (low mass) are the most common stars. Giants and supergiants are extremely rare. Bright, hot, blue main-sequence stars (high- mass) are very rare.

23. Shocks Triggering Star Formation 0 Henize 206 (infrared)

24. The Contraction of a Protostar

25. Protostellar Disks and Jets – Herbig-Haro Objects Disks of matter accreted onto the protostar (“accretion disks”) often lead to the formation of jets (directed outflows; bipolar outflows): Herbig-Haro objects

26. Herbig-Haro 34 in Orion Jet along the axis visible as red Lobes at each end where jets run into surrounding gas clouds

27. Motion of Herbig-Haro 34 in Orion Can actually see the knots in the jet move with time In time jets, UV photons, supernova, will disrupt the stellar nursery Hubble Space Telescope Image

28. The Source of Stellar Energy Stars produce energy by nuclear fusion of hydrogen into helium. In the sun, this happens primarily through the proton-proton (PP) chain

29. The Deaths and End States of Stars

30. The End of a Star’s Life When all the nuclear fuel in a star is used up, gravity will win over pressure and the star will die. High-mass stars will die first, in a gigantic explosion, called a supernova. Less massive stars will die in less dramatic events.

31. Evolution off the Main Sequence: Expansion into a Red Giant Hydrogen in the core completely converted into He: H burning continues in a shell around the core. He core + H-burning shell produce more energy than needed for pressure support Expansion and cooling of the outer layers of the star  red giant  “Hydrogen burning” (i.e. fusion of H into He) ceases in the core.

32. Expansion onto the Giant Branch Expansion and surface cooling during the phase of an inactive He core and a H-burning shell Sun will expand beyond Earth’s orbit!

33. High-mass stars evolved onto the giant branch Low-mass stars still on the main sequence Turn-off point HR Diagram of a Star Cluster

34. Red Dwarfs Recall: Stars with less than ~ 0.4 solar masses are completely convective.  Hydrogen and helium remain well mixed throughout the entire star.  No phase of shell “burning” with expansion to giant. Star not hot enough to ignite He burning. Mass

35. Sunlike Stars Sunlike stars (~ 0.4 – 4 solar masses) develop a helium core.  Expansion to red giant during H burning shell phase  Ignition of He burning in the He core  Formation of a degenerate C,O core Mass

36. White Dwarfs Degenerate stellar remnant (C,O core) Extremely dense: 1 teaspoon of white dwarf material: mass ≈ 16 tons!!! white dwarfs: Mass ~ M sun Temp. ~ 25,000 K Luminosity ~ 0.01 L sun Chunk of white dwarf material the size of a beach ball would outweigh an ocean liner!

37. Low luminosity; high temperature => White dwarfs are found in the lower center/left of the H-R diagram.

38. The Chandrasekhar Limit The more massive a white dwarf, the smaller it is.  Pressure becomes larger, until electron degeneracy pressure can no longer hold up against gravity. WDs with more than ~ 1.4 solar masses can not exist!

39. The Final Breaths of Sun-Like Stars: Planetary Nebulae The Helix Nebula Remnants of stars with ~ 1 – a few M sun Radii: R ~ 0.2 - 3 light years Expanding at ~10 – 20 km/s (  Doppler shifts) Less than 10,000 years old Have nothing to do with planets!

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

41. The Fate of our Sun and the End of Earth Sun will expand to a red giant in ~ 5 billion years Expands to ~ Earth’s orbit Earth will then be incinerated! Sun may form a planetary nebula (but uncertain) Sun’s C,O core will become a white dwarf

42. The Deaths of Massive Stars: Supernovae Final stages of fusion in high-mass stars (> 8 M sun ), leading to the formation of an iron core, happen extremely rapidly: Si burning lasts only for ~ 1 day. Iron core ultimately collapses, triggering an explosion that destroys the star: Supernova

43. The Crab Nebula–Supernova from 1050 AD Can see expansion between 1973 and 2001 –Kitt Peak National Observatory Images

44. The Famous Supernova of 1987: Supernova 1987A BeforeAt maximum Unusual type II supernova in the Large Magellanic Cloud in Feb. 1987

45. Type I and II Supernovae Core collapse of a massive star: type II supernova If an accreting white dwarf exceeds the Chandrasekhar mass limit, it collapses, triggering a type Ia supernova. Type I: No hydrogen lines in the spectrum Type II: Hydrogen lines in the spectrum

46. Neutron Stars Typical size: R ~ 10 km Mass: M ~ 1.4 – 3 M sun Density:  ~ 10 14 g/cm 3  Piece of neutron star matter of the size of a sugar cube has a mass of ~ 100 million tons!!! A supernova explosion of an M > 8 M sun star blows away its outer layers. The central core will collapse into a compact object of ~ a few M sun. Pressure becomes so high that electrons and protons combine to form stable neutrons throughout the object.

47. Discovery of Pulsars => Collapsing stellar core spins up to periods of ~ a few milliseconds. Angular momentum conservation => Rapidly pulsed (optical and radio) emission from some objects interpreted as spin period of neutron stars Magnetic fields are amplified up to B ~ 10 9 – 10 15 G. (up to 10 12 times the average magnetic field of the sun)

48. The Crab Pulsar Remnant of a supernova observed in A.D. 1054 Pulsar wind + jets

49. Black Holes Just like white dwarfs (Chandrasekhar limit: 1.4 M sun ), there is a mass limit for neutron stars: Neutron stars can not exist with masses > 3 M sun We know of no mechanism to halt the collapse of a compact object with > 3 M sun. It will collapse into a single point – a singularity: => A black hole!

50. Escape Velocity Velocity needed to escape Earth’s gravity from the surface: v esc ≈ 11.6 km/s. v esc Now, gravitational force decreases with distance (~ 1/d 2 ) => Starting out high above the surface => lower escape velocity. v esc If you could compress Earth to a smaller radius => higher escape velocity from the surface.

51. The Schwarzschild Radius => There is a limiting radius where the escape velocity reaches the speed of light, c: V esc = c R s = 2GM____ c2c2 R s is called the Schwarzschild radius. G = gravitational constant M = mass

52. Schwarzschild Radius and Event Horizon No object can travel faster than the speed of light  We have no way of finding out what’s happening inside the Schwarzschild radius. => nothing (not even light) can escape from inside the Schwarzschild radius  “Event horizon”

54. “Black Holes Have No Hair” Matter forming a black hole is losing almost all of its properties. black holes are completely determined by 3 quantities: mass angular momentum (electric charge)

55. The Gravitational Field of a Black Hole Distance from central mass Gravitational Potential The gravitational potential (and gravitational attraction force) at the Schwarzschild radius of a black hole becomes infinite.

56. General Relativity Effects Near Black Holes An astronaut descending down towards the event horizon of the black hole will be stretched vertically (tidal effects) and squeezed laterally.

57. General Relativity Effects Near Black Holes (II) Time dilation Event horizon Clocks starting at 12:00 at each point. After 3 hours (for an observer far away from the black hole): Clocks closer to the black hole run more slowly. Time dilation becomes infinite at the event horizon.

58. General Relativity Effects Near Black Holes (III) gravitational redshift Event horizon All wavelengths of emissions from near the event horizon are stretched (redshifted).  Frequencies are lowered.

59. Observing Black Holes No light can escape a black hole => Black holes can not be observed directly. If an invisible compact object is part of a binary, we can estimate its mass from the orbital period and radial velocity. Mass > 3 M sun => Black hole!