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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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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

  • X-ray emission is produced by hot gas bubbles and X-ray binaries


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


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


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


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


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


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


Dark Nebula

  • Associated with interstellar dust

  • Dust particles block the photons from the stars behind them

  • Dust will re-emit in the infra-red


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


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


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


Mapping Globular clusters


  • Our interpretation of the Milky Way

  • Disk is thin and wide

  • Note spiral arms and bar


We see our galaxy edge-on

Primary features: disk, bulge, halo, globular clusters


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


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


Orbits of stars in the bulge and halo have random orientations


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


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


Rotation

  • Possible models for rotation

  • Wheel or Merry-go-round

  • Planetary or Keplerian

  • Milky Way doesn’t rotate like either of these models


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


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


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


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


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


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


Stars slow down in the spiral arms

Density Waves


Much of star formation in disk happens in spiral arms

Whirlpool Galaxy


  • 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


Halo: No ionization nebulae, no blue stars

 no star formation

Disk: Ionization nebulae, blue stars  star formation


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


Infrared light from center

Radio emission from center


Swirling gas near center

Orbiting star near center


Stars appear to be orbiting something massive but invisible … a black hole?

Orbits of stars indicate a mass of about 4 million MSun


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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