1. Astro 10-Lecture 9: Properties of Stars How do we figure out the properties of stars? We’ve already discussed the tools: Light Gravity (virtually impossible to measure). Particles (might not get here). Now let’s apply them to stars!

2. Chabot Trip Let's pick a Friday (Apr 1? Apr 16?) Meet at a BART station –Need volunteers to drive Planetarium show and telescope viewing

3. Observation + geometry or physics

4. Chemical Composition Presence of Absorption lines of a particular element indicates the presence of that element in the star! Absence of a spectral line doesn't necessarily mean an element is absent.

5. Chemical Composition

6. Temperature Wavelength of Spectral Peak + Blackbody Radiation Absorption Lines + Atomic Physics

7. Distance (1) Trigonometric Parallax – You’ve all used it! Animation lec9_pix\parallax.mpg

8. Distance (1)

9. Distance (3) Trigonometric Parallax – useful to 50pc (ground) and 500 pc (space) Parsec (pc) = Distance of a Star with a Parallax of 1 (one) arcsecond (ParSec) 1 pc is a little over 3 light years!

10. Space Velocity (1) Velocity = Speed + Direction Space Velocity has 2 components  Radial Velocity (Towards/Away)  Transverse Velocity (sideways) Transverse Velocity: PROPER MOTION + DISTANCE Animation

11. Space Velocity (2) Radial Velocity: DOPPLER EFFECT carhorn.wav

12. Space Velocity (2)

15. Space Velocity (3) Radial Velocity: Doppler Effect

16. ConcepTest Two stars lie in the same area of the sky. Star Gern has a parallax measurement of 1 arcsecond, while Star Zora has a parallax measurement of 0.5 arcseconds. – a) Star Gern is closer to us than star Zora – b) Star Gern has a larger space velocity than star Zora – c) Star Gern and Star Zora are at the same distance – d) Star Gern and Star Zora have the same temperature

17. Apparent Brightness vs. Luminosity Apparent Brightness: Energy we intercept per unit area per unit time (how bright it appears) Luminosity: Energy emitted per unit time (how bright it really is) Inverse Square Law: Projector Demo

18. The inverse square law Brightness proportional to 1/d 2 Demo LUMINOSITY: APPARENT BRIGHTNESS + DISTANCE

19. Inverse Square Law

20. Hertzprung-Russell (H-R) Diagram A Plot of Temperature vs. Luminosity

21. HR Diagram Notice that the Temperature axis is reversed! (So is the magnitude axis, but we don’t use it) NOTE HUGE RANGE OF LUMINOSITIES!

22. MASS! (1) Period/Size of orbits are related to MASS by Newton’s version of Kepler’s Third Law Qualitatively, if two masses are orbiting about one another very rapidly, then the gravity between them must be stronger than if they were orbiting more slowly. SUM of MASSES: Orbital Period + Orbital Size + GRAVITY

23. MASS – Binary Stars (2) We can get stellar masses from observations of Binary Stars  Visual Binary (see the two stars move about one another on the sky)  Spectroscopic Binary (see the motion due to Doppler shifts of spectral lines)  Eclipsing Binary (see the light from one star periodically blocked by the other)

24. Visual Binaries Distance + angle measurement => orbital size Period + orbital size + gravity => sum of masses Center of mass determination gives individual masses

25. Spectroscopic Binaries Orbital velocity determined by Doppler shifts of lines in spectrum (OH 69) spbin.mov Period + Maxumum orbital velocity gives ~size of orbit INCLINATION PROBLEM Some stars in Big Dipper are Binaries!

26. Spectroscopic Binaries (2)

27. Eclipsing Binaries One star passes in front of the other at some point during the orbit, reducing the light that reaches us OH 70 eclbin.mov Eclipsing + Spectroscopic Binary => NO INCLINATION PROBLEMS

28. MASS RECAP Newton’s Laws of Gravity say that if we know 1) size of orbit 2) period of orbit then we can find the total mass of the system Size of orbit: need either distance, or eclipsing spectroscopic binary To find individual masses, must know where the Center of Mass of the system is Stellar masses are 0.01 to 100 times Sun’s mass

29. Mass-Luminosity Relation

30. Radius (size) from Binaries (1) In an eclipsing spectroscopic binary system, we can find the RADIUS of the stars too! Time spent in eclipse + orbital velocity of star (from Doppler) => SIZE OF STAR

31. Radius from Blackbody Radiation (2) Blackbody radiation law says that the energy emitted / area / time by the star is determined only by its TEMPERATURE So if we can determine the LUMINOSITY (energy emitted / time) of the Star, we can combine this with its TEMPERATURE to determine the RADIUS TEMPERATURE + LUMINOSITY + BLACKBODY RADIATION => RADIUS

32. Radius from Blackbody Radiation (2) Giants: ~10 x size of sun (~1000 x size of Earth) Supergiants: ~10-1000 x size of sun (~1000-100,000 x size of Earth) White Dwarfs: ~ size of Earth

33. Radius from Blackbody Radiation (2) L=4  R 2  T 4 Giants: ~10 x size of sun (~1000 x size of Earth) Supergiants: ~10-1000 x size of sun (~1000-100,000 x size of Earth) White Dwarfs: ~ size of Earth

34. Now What? Notice that most of these quantities rely in some way upon a determination of DISTANCE Remember Trigonometric Parallax is only good to ~500 pc, while the Milky Way Galaxy is ~17,000 pc across! How do we learn anything about more distant stars?

35. Spectroscopic Parallax (1) Previously: Measurement + geometry or physics => Quantity NOW – Let’s USE what we’ve learned to bootstrap our way to more distant stars! Suppose we KNEW the intrinsic luminosity of a star – then a measure of its apparent brightness would tell us its DISTANCE (remember the INVERSE SQUARE LAW?)

36. Spectroscopic Parallax (2) If all stars were on the “Main Sequence” in the HR diagram, then a measurement of the TEMPERATURE of the star would allow you to determine its LUMINOSITY from the H-R diagram LUMINOSITY + APPARENT BRIGHTNESS + INVERSE SQUARE => DISTANCE Notice that this only works AFTER we have found the luminosities of many stars other ways, and “calibrated” the H-R diagram

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38. Spectroscopic Parallax (3) NOTE: We’re assuming more distant stars are just like nearby ones! BUT WAIT! Not all stars lie on the Main Sequence Subtle differences in the widths of the star’s absorption lines can determine its “Luminosity Class” (WD, MS, giant, supergiant) Measure spectrum + blackbody + atomic physics => TEMP and LUMINOSITY CLASS + CALIBRATED HR DIAGRAM => LUMINOSITY + APPARENT BRIGHTNESS + INV SQ => DISTANCE

39. What does the Population of Stars look like? What makes a star shine (model)? How can we TEST this model with observation?

40. Observation + geometry or physics

41. ConcepTest By looking at the spectra of two stars, we learn that they are both main sequence stars, and they have the same temperature. 1) If we can measure the distance to ONE of the stars using trigonometric parallax, can we find the distance to the other star? (A=yes, B=no) 1) If we could not measure the distance to ANY stars using trigonometric parallax, can we find the luminosity of these stars? (A=yes, B=no)

42. Population of Stars The Sun isn’t special! Nearest star is ~ 4 ly away Temperatures: 2,000-30,000K (sun 5800) Luminosities: 1/100,000 to > 1,000,000 x sun Fall into “classes” on the H-R diagram Main sequence (sun), white dwarfs, red giants, supergiants

43. Population of Stars (2) Radii: WD ~ Earth-sized (1/100 of Sun) Giants ~ 10-100 x size of sun (~Earth orbit in our scale model of the solar system) Supergiants ~ 100-1000 x size of sun Mass: ~0.1 Msun to 55-100 Msun Mass + Radius => Density (DEMO) MS: density sun ~ 1g/cm 3 ~ density water Giants: 0.1 – 0.01 x density sun Supergiants: 0.001 – 0.000001 x density sun WD: ~ 3 000 000 x density sun (1 tsp ~ 15 tons on Earth)

44. Mass-Luminosity Relation For MAIN-SEQUENCE STARS ONLY: A relationship between MASS and LUMINOSITY Most luminous main-sequence stars are also the most massive ( (L ~ M 3.5 )

45. POPULATION STATISTICS What stars do we see as bright in the night sky? LUMINOUS ONES What stars are the nearest? DIM (RED) ONES How many stars of each kind per cubic parsec? LUMINOUS RARE, NEAREST DIM

46. Comparing HR Diagrams for nearest and brightest stars Nearest Stars Brightest Stars

47. IN-CLASS EXERCISE