1. A105 Stars and Galaxies  This week’s units: 70, 71, 72, 73  News Quiz Today  Milky Way homework due Thursday  3 observing events Today’s APODAPOD

2. Announcements… Kirkwood Obs. open –Weds night 7-9 PM Rooftop Thursday 8 PM Transit of Mercury Weds –2:15 – 5:15 –Kirkwood & Sample Gate

3. Transit of Mercury Or view it online at: www.exploratorium.edu/transit/

4. Introducing: The Milky Way Our very own spiral galaxy

6. Four Galaxies similar to the MW Barred spirals (seen face-on)

7. The Andromeda Galaxy Almost a twin of the Milky Way… Just bigger

8. Exploring the Milky Way Virtual Reality All-Sky Milky Way Panorama

9. The Milky Way…. Halo Dwarf Spheroidal Companions Dark Matter Corona Bulge Disk Halo

10. Where is the Center of the Milky Way?

11. Measuring the True Size and Shape of the Milky Way The discovery of certain types of variable stars allowed Harlow Shapley to determine the distances to globular star clusters Globular clusters concentrate near the center of the galaxy.

12. Globular Cluster Locations The Galactic Center The Sun The distance to the Galactic Center is about 8 kiloparsecs (8,000 parsecs), or about 26,000 light years

13. Key Ideas The Milky Way is a spiral galaxy The Galaxy is shaped like a disk The Sun is located at the inner edge of a spiral arm about 2/3 of the way out from the center to the edge The main components of the Galaxy are the disk, the bulge, and the halo We can measure the mass of the Galaxy from the orbits of stars

14. THE MILKY WAY Draw two sketches of the Milky Way from different perspectives Add as many details as you can

15. Milky Way Factoids The Sun orbits the center of the Galaxy –moving in a direction toward Cygnus –speed of about 220 kilometers/second –One orbit takes about 240 MILLION years The mass of the Galaxy is about 2x10 11 times the mass of the Sun

16. The Milky Way – Review Vital Stats Consists of 100 billion stars. Stars are distributed in a central bulge, a huge disk, and a galactic halo surrounding both. The diameter of the disk is 30kpc (100,000 light years). The thickness of the disk is only 300pc (1000 light years) on average. The total detectable mass is 200 billion solar masses.

17. Our Local Neighborhood The Sun is located on the outskirts. Most stars in our neighborhood are cool, low mass stars There are no massive (O or B) stars nearby The interstellar gas in our neighborhood is still quite hot  It is a graveyard of recent massive star deaths.

18. Galactic Inhabitants Stars (of all masses) – disk/bulge Star clusters – open clusters (near the disk), globular clusters in the halo Clouds – giant molecular clouds, H I clouds, H II regions (disk) Nebulae – reflection nebulae, emission nebulae, nova/supernova remnants, planetary nebulae – disk

19. The Disk –Gas – ionized hydrogen (H II), atomic hydrogen (H I), molecular hydrogen (densest and coldest), stellar ejecta –Dust –Stars and failed stars (brown dwarfs) –Stellar remnants – black holes, neutron stars, white dwarfs The Halo –Is virtually gas free which implies little star formation and chemical enrichment –Consists mostly of old, metal-poor stars (for example, in the globular clusters)

20. Stellar “Populations” Stars formed at a particular “epoch” of the history of the Milky Way share similar properties such as composition and motion.

21. Structure of the Disk

22. What Sustains the Spiral Pattern? The stars in the galaxy revolve around the galactic center due to gravity The galactic disk rotates differentially – stars near the center move faster than those farther away This produces a spiral structure but should quickly wind up after a few rotations and disappear What then preserves the arms?

23. One origin of density waves

24. The Density Wave Theory According to this theory, the spiral arms are not material but are rather waves or ripples which cause greater concentrations of stars and interstellar dust and gas. Stars move in special, precessing elliptical orbits which gives rise to the spiral pattern. The spiral pattern moves as a shock through the galaxy, compressing gas into molecular clouds, promoting star formation at the trailing edges.

25. The Milky Way

26. Origin of the Milky Way I A huge, million- parsec-sized blob of gas begins to contract under gravity. The first stars and star clusters form.

27. Origin of the Milky Way II The rotating cloud of gas begins to contract toward its equatorial plane.

28. Origin of the Milky Way III Stars and clusters are left behind in the “halo” as the gas cloud flattens.

29. Origin of the Milky Way IV IV Stars and clusters formed in the flattened cloud remain in the newly formed “disk”

30. Origin of the Milky Way V The disk is now very thin, and the bulge has formed Throughout the process smaller galaxies are cannibalized as the Milky Way grows

31. The Milky Way Is Still Growing Nearby dwarf galaxy discovered in 1994 in the direction of Sagittarius Discovered by radial velocity Distance about 88,000 light years Merging with the Milky Way

32. Orbits the Milky Way Orbital period about a billion years “Tidal stream” of stars from Sagittarius circles the Milky Way Sagittarius may contain significant dark matter Sagittarius Tidal Stream

33. Yet Another New Galaxy! Canis Major Dwarf Nearest galaxy to the Milky Way (yet discovered…) 25,000 light years from the Sun 44,000 light years from the center of the Milky Way Discovered with IR light (hidden behind dust in the MW’s disk)

34. Tidal Streams from CMa Wrap around the Milky Way

35.  Read Units 70, 71, 72, 73  Milky Way HW Due THURS.  3 observing events available