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Lecture 21 Cosmological Models

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Title: Lecture 21 Cosmological Models


1
Lecture 21Cosmological Models
  • ASTR 340
  • Fall 2006
  • Dennis Papadopoulos

2
Spectral Lines - Doppler
3
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4
Doppler Examples
5
Doppler Examples
6
Expansion Redshifts
z2 three times, z10, eleven times
7
Expansion Redshifts
8
Expansion - Example
9
Current Record Redshift
10
Hubbleology
  • Hubble length DHc/H ,
  • Hubble sphere Volume enclosed in Hubble sphere
    estimates the volume of the Universe that can be
    in our light-cone it is the limit of the
    observable Universe. Everything that could have
    affected us
  • Every point has its own Hubble sphere
  • Look-back time Time required for light to travel
    from emission to observation

11
Gravitational Redshift
12
Interpretation of Hubble law in terms of
relativity
  • New way to look at redshifts observed by Hubble
  • Redshift is not due to velocity of galaxies
  • Galaxies are (approximately) stationary in space
  • Galaxies get further apart because the space
    between them is physically expanding!
  • The expansion of space, as R(t) in the metric
    equation, also affects the wavelength of light
    as space expands, the wavelength expands and so
    there is a redshift.
  • So, cosmological redshift is due to cosmological
    expansion of wavelength of light, not the regular
    Doppler shift from local motions.

13
Relation between z and R(t)
  • Using our relativistic interpretation of cosmic
    redshifts, we write
  • Redshift of a galaxy is defined by
  • So, we have

14
Hubble Law for nearby (zlt0.1) objects
  • Thus
  • where Hubbles constant is defined by
  • But also, for comoving coordinates of two
    galaxies differing by space-time interval
  • dR(t)?Dcomoving , have
  • v Dcomoving ? ?R/?t(d/R)?(?R/?t)
  • Hence v d? H for two galaxies with fixed
    comoving separation

15
Peculiar velocities
  • Of course, galaxies are not precisely at fixed
    comoving locations in space
  • They have local random motions, called peculiar
    velocities
  • e.g. motions of galaxies in local group
  • This is the reason that observational Hubble law
    is not exact straight line but has scatter
  • Since random velocities do not overall increase
    with comoving separation, but cosmological
    redshift does, it is necessary to measure fairly
    distant galaxies to determine the Hubble constant
    accurately

16
Distance determinations further away
  • In modern times, Cepheids in the Virgo galaxy
    cluster have been measured with Hubble Space
    Telescope (16 Mpc away)

Virgo cluster
17
Tully-Fisher relation
  • Tully-Fisher relationship (spiral galaxies)
  • Correlation between
  • width of particular emission line of hydrogen,
  • Intrinsic luminosity of galaxy
  • So, you can measure distance by
  • Measuring width of line in spectrum
  • Using TF relationship to work out intrinsic
    luminosity of galaxy
  • Compare with observed brightness to determine
    distance
  • Works out to about 200Mpc (then hydrogen line
    becomes too hard to measure)

18
Hubble time
  • Once the Hubble parameter has been determined
    accurately, it gives very useful information
    about age and size of the expanding Universe
  • Recall Hubble parameter is ratio of rate of
    change of size of Universe to size of Universe
  • If Universe were expanding at a constant rate, we
    would have ?R/?tconstant and R(t) t?(?R/?t)
    then would have H (?R/?t)/R1/t
  • ie tH1/H would be age of Universe since Big Bang

19
Modeling the Universe
Chapter 11
20
BASIC COSMOLOGICAL ASSUMPTIONS
  • Germany 1915
  • Einstein just completed theory of GR
  • Explains anomalous orbit of Mercury perfectly
  • Schwarzschild is working on black holes etc.
  • Einstein turns his attention to modeling the
    universe as a whole
  • How to proceed its a horribly complex problem

21
How to make progress
  • Proceed by ignoring details
  • Imagine that all matter in universe is smoothed
    out
  • i.e., ignore details like stars and galaxies, but
    deal with a smooth distribution of matter
  • Then make the following assumptions
  • Universe is homogeneous every place in the
    universe has the same conditions as every other
    place, on average.
  • Universe is isotropic there is no preferred
    direction in the universe, on average.

22
  • There is clearly large-scale structure
  • Filaments, clumps
  • Voids and bubbles
  • But, homogeneous on very large-scales.
  • So, we have the
  • The Generalized Copernican Principle there are
    no special points in space within the Universe.
    The Universe has no center!
  • These ideas are collectively called the
    Cosmological Principles.

23
Key Assumptions
24
Riddles of Conventional Thinking
25
Stability
26
GR vs. Newtonian
27
Newtonian Universe
28
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29
Expanding Sphere
30
Fates of Expanding Universe
31
Spherical Universe
32
Friedman Universes
33
Einsteins Greatest Blunder
34
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35
THE DYNAMICS OF THE UNIVERSE EINSTEINS MODEL
  • Einsteins equations of GR

G describes the space-time curvature (including
its dependence with time) of Universe heres
where we plug in the RW geometries.
T describes the matter content of the Universe.
Heres where we tell the equations that the
Universe is homogeneous and isotropic.
36
  • Einstein plugged the three homogeneous/isotropic
    cases of the FRW metric formula into his
    equations of GR to see what would happen
  • Einstein found
  • That, for a static universe (R(t)constant), only
    the spherical case worked as a solution to his
    equations
  • If the sphere started off static, it would
    rapidly start collapsing (since gravity attracts)
  • The only way to prevent collapse was for the
    universe to start off expanding there would then
    be a phase of expansion followed by a phase of
    collapse

37
  • So Einstein could have used this to predict that
    the universe must be either expanding or
    contracting!
  • but this was before Hubble discovered expanding
    universe (more soon!) everybody thought that
    universe was static (neither expanding nor
    contracting).
  • So instead, Einstein modified his GR equations!
  • Essentially added a repulsive component of
    gravity
  • New term called Cosmological Constant
  • Could make his spherical universe remain static
  • BUT, it was unstable a fine balance of opposing
    forces. Slightest push could make it expand
    violently or collapse horribly.

38
  • Soon after, Hubble discovered that the universe
    was expanding!
  • Einstein called the Cosmological Constant
    Greatest Blunder of My Life!
  • .but very recent work suggests that he may have
    been right (more later!)

39
Sum up Newtonian Universe
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