1. 14.2 Galactic Recycling Our Goals for Learning How does our galaxy recycle gas into stars? Where do stars tend to form in our galaxy?

2. How does our galaxy recycle gas into stars?

3. Star-gas-star cycle Recycles gas from old stars into new star systems

4. High-mass stars have strong stellar winds that blow bubbles of hot gas

5. Lower mass stars return gas to interstellar space through stellar winds and planetary nebulae

6. X-rays from hot gas in supernova remnants reveal newly- made heavy elements

7. Supernova remnant cools and begins to emit visible light as it expands New elements made by supernova mix into interstellar medium

8. Multiple supernovae create huge hot bubbles that can blow out of disk; gas cooling in the halo can rain back down on disk.

9. Atomic hydrogen gas forms as hot gas cools, allowing electrons to join with protons. Molecular clouds form next, after gas cools enough to allow to atoms to combine into molecules

10. Molecular clouds in Orion Composition: Mostly H 2 About 28% He About 1% CO Many other molecules

11. Gravity forms stars out of the gas in molecular clouds, completing the star-gas- star cycle

12. Radiation from newly formed stars is eroding these star- forming clouds

13. Summary of Galactic Recycling Stars make new elements by fusion Dying stars expel gas and new elements, producing hot bubbles (~10 6 K) Hot gas cools, allowing atomic hydrogen clouds to form (~100-10,000 K) Further cooling permits molecules to form, making molecular clouds (~30 K) Gravity forms new stars (and planets) in molecular clouds Gas Cools

14. We observe star-gas-star cycle operating in Milky Way’s disk using many different wavelengths of light

15. Infrared light reveals stars whose visible light is blocked by gas clouds Infrared Visible

16. X-rays are observed from hot gas above and below the Milky Way’s disk X-rays

17. 21-cm radio waves emitted by atomic hydrogen show where gas has cooled and settled into disk Radio (21cm)

18. Radio waves from carbon monoxide (CO) show locations of molecular clouds Radio (CO)

19. Long-wavelength infrared emission shows where young stars are heating dust grains IR (dust)

20. Gamma rays show where cosmic rays from supernovae collide with atomic nuclei in gas clouds

21. Where do stars tend to form in our galaxy?

22. Ionization nebulae are found around short-lived high-mass stars, signifying active star formation

23. Reflection nebulae scatter the light from stars. Why do reflection nebulae look blue, even when the stars near them aren't blue?

24. Reflection nebulae scatter the light from stars Why do reflection nebulae look bluer than the nearby stars? For the same reason that our sky is blue!

25. What kinds of nebulae do you see?

26. Disk: Ionization nebulae, blue stars  star formation Halo: No ionization nebulae, no blue stars  no star formation

27. Much of star formation in disk happens in spiral arms Whirlpool Galaxy

28. Much of star formation in disk happens in spiral arms Whirlpool Galaxy Ionization Nebulae Blue Stars Gas Clouds

29. Spiral arms are waves of star formation

30. Gas clouds get squeezed as they move into spiral arms Squeezing of clouds triggers star formation Young stars flow out of spiral arms

31. 14.4 The Mysterious Galactic Center Our Goals for Learning What lies in the center of our galaxy?

32. Activity 33, page 113-115 –Question 3A: pinpoint the location of the center of our galaxy using the two longest acceleration vectors shown in Figure 1.

33. Galactic center in infrared lightGalactic center in radio

34. Strange radio sources in galactic center Galactic center in radio

35. Stars at galactic center Strange radio sources in galactic center

36. Stars appear to be orbiting something massive but invisible … a black hole. Orbits of stars indicate a mass of about 4 million M Sun

37. What have we learned? How does our galaxy recycle gas into stars? Stars are born from the gravitational collapse of gas clumps in molecular clouds. Near the ends of their lives, stars more massive than our Sun create elements heavier than hydrogen and helium and expel them into space via supernovae and stellar winds. The supernovae and winds create hot bubbles in the interstellar medium, but the gas within these bubbles gradually slows and cools as they expand. Eventually, this gas cools enough to collect into clouds of atomic hydrogen. Further cooling allows atoms of hydrogen and other elements to collect into molecules, producing molecular clouds.These molecular clouds then form stars, completing the star–gas–star cycle. Stacie Kent: Insert thumbnail of 14.8

38. What have we learned? Where do stars tend to form in our galaxy? Active star-forming regions, marked by the presence of hot, massive stars and ionization nebulae, are found preferentially in spiral arms. The spiral arms represent regions where a spiral density wave has caused gas clouds to crash into each other, thereby compressing them and making star formation more likely.

39. What have we learned? What lies in the center of our galaxy? Motions of stars near the center of our galaxy suggest that it contains a black hole about 3 to 4 million times as massive as the Sun. The black hole appears to be powering a bright source of radio emission known as Sgr A*.