1. The Sun and Stars Chapters 10 and 11

2. Topics the Sun –Features –Structure –Composition –How do we know? Stars –brightness and luminosity –distance –temperature –mass –classification

3. Sun Photosphere –the bright disc we see as “the Sun” –the “surface”of the Sun –causes the absorption lines in the Sun’s spectrum (called Fraunhoffer lines) –temperature 5800 K –mostly hydrogen (94%) and helium (5.9%) Chromosphere –thin layer above the photosphere –7000 K - 15,000 K Corona –halo of high energy gas, very hot (2 MK) –emits radiation (thus we can see emission lines), mostly x-rays

4. Sun

5. Activity on the Sun sunspots –cyclic –cooler region of the photosphere –related to the Sun’s magnetic field prominences solar flares –solar storm –emits radiation and particles –high temperature (>5 MK) –affect radio communications on Earth

6. Sunspot cycle 11 year average cycle Time between maxima can be as long as 15 years or as short as 7 years. Solar activity may affect Earth’s climate, but the mechanisms are unknown.

7. From http://sohowww.nascom.nasa.gov/ A comparison of two EIT images almost two years apart illustrates how the level of solar activity has increased significantly. The Sun attains its expected sunspot maximum in the year 2000. These images are captured using Fe IX-X 171 Å emission showing the solar corona at a temperature of about 1.3 million K. Many more sunspots, solar flares, and coronal mass ejections occur during the solar maximum. The numerous active regions and the number/size of magnetic loops in the recent image shows the increase.

8. General Theory of Relativity Newton’s theory of gravitation does not explain everything –bending of light near massive objects (light is seemingly attracted to mass?) –precession of the perihelion of Mercury (now it’s known that the perihelions of other planets precess as well) Local space-time is curved by the presence of mass –light (and everything else) travels in a curved space-time. –objects left to themselves travel in straight lines –a straight-line on a curved surface is a geodesic, or great circle Early evidence that Einstein was right was the observation that light from a star was bent as it passed near the Sun (this could only be seen during a total solar eclipse of course)

9. Are other stars like our Sun? Let’s measure apparent brightness –the amount of radiation we receive per second luminosity –the amount of radiation emitted by the star per second distance temperature composition

10. Brightness and Luminosity Brightness: How bright a star appears. Luminosity: How much light the star is actually giving off. Apparent MagnitudeAbsolute Magnitude

11. Apparent magnitude scale Introduced by Hipparchus (160-127 B.C.) –Vega (0), Venus (-4), Sun (-26.8), Moon (-12.6), Faintest objects observed with HST (+30) What does it measure? –measures ratios of actual amount of light energy received –receive 2.5x more energy from a mag. 1 star than a mag. 2 star –difference of 5 magnitudes is 100x difference in received energy

12. How does it work? 7.8 6.8 5.8 4.8 3.8 2.5 X 2.5X2.5 = 6.25 X 2.5 X 15.6 X 2.5 X 39.1 X 2.8 2.5 X 100 XDifference of 5

13. Practice Rigil Kentaurus (-0.01) Spica (+1.0) Which looks brighter? How much more light do we receive from it? One level of magnitude means 2.5 times more light received!!

14. But... Spica is actually more than 1000x more luminous than Rigil Kentaurus!! If Spica is putting out more light, why might it appear dimmer in the sky?

15. Apparent brightness apparent brightness diminishes with distance inverse-square law (brightness diminishes as 1/D 2 )

19. Practice Both stars have apparent magnitude +4 AB What can you conclude about their luminosities? 4 ly12 ly How do we find distance?

20. Parallax Parallax - the apparent change in position of an object due to the change in position of the observer. JanuaryJune

21. 12345678 12345678 Observer

22. 12345678 12345678

23. 12345678 12345678 Parallax But why would stars do this? Would an object here appear to move more or less?

24. 1 AU JanJuly p Is p larger or smaller for a star farther away?

25. 1 AU TRUE POSITION APPARENT POSITION Earth (Jan) Earth (Jul) p

26. 1 AU TRUE POSITION APPARENT POSITION Earth (Jan) Earth (Jul) p

27. TRIANGULATION the smaller the parallax angle the greater the distance one arc second=1/3600 of 1 degree distance from Earth to a star where p=1 arc second is called the parsec a parsec=3.26 ly

28. Parallax Results: Closest star is Proxima Centauri, which is located at 1.3 parsecs. Method good to about 250 parsecs! Gives knowledge of fraction of one percent of stars in Milky Way About 1/100 of diameter of galaxy!!

29. Hipparcos Satellite HIgh Precision PARallax COllecting Satellite (1989-1993)

30. Hipparcos Target: 118,000 stars Magnitude limit: 12.5 Resolution: 0.001 arcsecond!!! (about 200 parsecs)

31. Practice Consider two stars (X and Y). If star X is 3 parsecs away and star Y is 5 parsecs away, which has the greater parallax angle? a) Star X b) Star Y c) Not enough information

32. Comparing brightness How can we compare brightness if stars are at varying distances? Calculate brightness as if the star is at a distance of 10 parsecs (33 ly). This is called its absolute magnitude.

33. What magnitude would Antares (-0.1) appear if it were at a distance of 10 parsecs? Take the current distance to be 100 parsecs. Are we expecting a number greater or less than -0.1? 10 x closer = _____ x brighter100 How many magnitudes is 100 x brighter? 1 mag = 2.5x 5 mag = 100x absolute magnitude = -0.1  5 -= -5.1 brighter or dimmer?

34. Checkpoint What do we know now? –apparent brightness is different than luminosity and depends on distance to the star –for the nearest stars, we can use parallax to determine distance –we describe apparent brightness with the apparent magnitude scale and luminosity with the absolute magnitude scale What else do we want to measure?

35. Temperature temperature can be directly measured for a blackbody by plotting the brightness vs. wavelength (i.e. a blackbody curve). temperature affects the color of the star peak wavelength depends on temperature

36. Blackbody curves

37. Temperature and brightness As T increases, the wavelength for peak brightness decreases. As T increases, the brightness increases.

38. How does temperature affect aborption spectra? Absorption lines tell us about the composition of the stars. Stars were originally grouped according to similar absorption spectra Later we realized that the intensity (i.e. darkness) of certain H lines were indicative of temperatures

39. O B A F G K M

40. Classification of stars by brightness Each type is further divided into 10 subtypes (0-9)

41. H-R diagram A graph of stars’ luminosity (or absolute magnitude since they are related) vs. temperature (or spectral type since they are related) short for Hertzsprung-Russell diagram

42. same luminosity

43. very large

44. RED GIANTS Cool but VERY BRIGHT!Cool but VERY BRIGHT! Betelgeuse: 3500 K (10% as bright/unit area as Sun) but 100,000 times as luminous--must have 1 million times the areaBetelgeuse: 3500 K (10% as bright/unit area as Sun) but 100,000 times as luminous--must have 1 million times the area radius must be 1000x that of Sun!radius must be 1000x that of Sun!

46. same temperature

47. very large very small

48. Globular Cluster in Scorpius