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The Milky Way

The Milky Way Dr Bryce 29:50 Class notices The Milky Way galaxy appears in our sky as a faint band of light “All sky view” The Milky Way in Visible light The Milky Way at 21cm wavelength Neutral hydrogen in confined to the plane of the Milky Way The Milky Way at X-ray Wavelengths

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The Milky Way

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  1. The Milky Way Dr Bryce 29:50

  2. Class notices

  3. The Milky Way galaxy appears in our sky as a faint band of light

  4. “All sky view” • The Milky Way in Visible light

  5. The Milky Way at 21cm wavelength • Neutral hydrogen in confined to the plane of the Milky Way

  6. The Milky Way at X-ray Wavelengths • X-ray emission is produced by hot gas bubbles and X-ray binaries

  7. Interstellar Medium • Can both absorb and emit light • Most of the interstellar medium is gas and it is easiest to observe when it forms an emission cloud/nebula • Good examples of this include the Orion Nebula • Because the gas is predominantly hydrogen we see lines associated with atomic or ionized hydrogen

  8. HII regions • “H two” • Strong emission lines • A central hot star emits UV photons which ionize the hydrogen • When an electron is recaptured by a proton the HII line is emitted

  9. HII regions • Require a hot star to have formed in a molecular cloud • The hotter the star the larger the HII region can be • HII regions tend to be red – see the Rosette Nebula

  10. 21cm line • Associated with the lowest energy level of Hydrogen • Doesn’t involve the hydrogen atom interacting with another photon so we can “see” this line anywhere in space

  11. Interstellar gas temperature • Molecular clouds are dense and at low temperatures (~10K) • Interstellar gas is much less dense and much warmer (~10,000K) • We also see very hot (~1 million K) gas from Supernova shock waves, it is these regions that are responsible for the X-ray bubbles

  12. Gas recycling • Stars make new elements by fusion • Dying stars expel gas and new elements, producing hot bubbles (~106 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

  13. Dark Nebula • Associated with interstellar dust • Dust particles block the photons from the stars behind them • Dust will re-emit in the infra-red

  14. The development of our Model • Galileo first observed that the Milky Way is made up of stars and many astronomers have tried to map it • For example Herschel used star counts, see below

  15. Early models • Were incorrect as they didn’t include the effects of interstellar dust which will dim starlight (this effect is called extinction) and interstellar reddening • It is for these reasons that we actually find it easier to study other galaxies rather than the galaxy in which we live

  16. Globular clusters • We know from our H-R diagrams that globular clusters are old • One way to map the Milky Way is to consider the distribution of globular clusters

  17. Mapping Globular clusters

  18. Our interpretation of the Milky Way • Disk is thin and wide • Note spiral arms and bar

  19. We see our galaxy edge-on Primary features: disk, bulge, halo, globular clusters

  20. If we could view the Milky Way from above the disk, we would see its spiral arms

  21. Stars in the disk all orbit in the same direction with a little up-and-down motion

  22. Orbits of stars in the bulge and halo have random orientations

  23. Sun’s orbital motion (radius and velocity) tells us mass within Sun’s orbit: 1.0 x 1011MSun Sun is about 8kpc from the galactic centre

  24. Orbital Velocity Law • The orbital speed (v) and distance from the galactic centre (d) of an object on a circular orbit around the galaxy tells us the mass (M) within that orbit

  25. Rotation • Possible models for rotation • Wheel or Merry-go-round • Planetary or Keplerian • Milky Way doesn’t rotate like either of these models

  26. Milky Way’s rotation Curve • Is “flat” • This means that the distribution of mass in the Milky Way continues outwards past the luminous material (stars) • The dark matter could be brown dwarfs, white dwarfs, Jupiters, Black holes or elementary particles, they are not emitting light but they are exerting gravitational influence

  27. The visible portion of a galaxy lies deep in the heart of a large halo of dark matter

  28. We can measure rotation curves of other spiral galaxies using the Doppler shift of the 21-cm line of atomic H

  29. Spiral galaxies all tend to have flat rotation curves indicating large amounts of dark matter

  30. Gravitational microlensing • A dark object in the galactic halo (MACHO) could act as a lens because of the curvature of spacetime around it. • Black holes would be the strongest type of microlens

  31. Spiral Structure • We can easily observe spiral arms in other galaxies but within the Milky Way our view is hindered by the effects of interstellar gas and dust

  32. Stars slow down in the spiral arms Density Waves

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

  34. Spiral arms are waves of star formation • Gas clouds get squeezed as they move into spiral arms • Squeezing of clouds triggers star formation • Young stars flow out of spiral arms

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

  36. Halo Stars: 0.02-0.2% heavy elements (O, Fe, …), only old stars Halo stars formed first, then stopped Disk Stars: 2% heavy elements, stars of all ages Disk stars formed later, kept forming

  37. Infrared light from center Radio emission from center

  38. Swirling gas near center Orbiting star near center

  39. Stars appear to be orbiting something massive but invisible … a black hole? Orbits of stars indicate a mass of about 4 million MSun

  40. X-ray flares from galactic center suggest that tidal forces of suspected black hole occasionally tear apart chunks of matter about to fall in

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