The fate of the universe

Сентябрь 6, 2022

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The fate of the universe

Содержание

2. The Fate of the Universe Depends on how much mass and energy there is in the
3. The Fate of the Universe Depends on how much mass and energy there is in the
4. The Fate of the Universe Depends on how much mass and energy there is in the
5. Comparison to Earth’s Gravity
6. The Fate of the Universe Depends on how much mass and energy there is in the
7. The Fate of the Universe Depends on how much mass and energy there is in the
8. Possible explanation for the acceleration: vacuum pressure (cosmological constant), more generically called dark energy. In reality,
9. Type I supernovae can be used to measure the behavior of distant galaxies. In a decelerating
10. However, when we look at the data, we see that it corresponds not to a decelerating
11. The Critical Density The amount of mass needed to just barely make the Universe closed is
12. Density and the Fate of the Universe If Ω > 1, the Universe will eventually collapse.
13. If the density is low, the universe will expand forever. If it is high, the universe
14. The answer to this question lies in the actual density of the Universe. Measurements of luminous
15. However, the best estimates for the amount of dark matter needed to bind galaxies in clusters,
16. Dark Energy and The Cosmological Constant Curiously, Einstein had introduced this idea decades before in order
17. I have drawn these curves starting from the Big Bang, but we should really draw them
18. If space is homogenous, there are three possibilities for its overall geometry: Closed – this is
19. These three possibilities are illustrated here. The closed geometry is like the surface of a sphere;
20. Summary of the Possible Geometries
21. Refining the Big Bang Model II: The Flatness Problem We don’t yet know the geometry of
22. Inflation can also solve the flatness problem. A heavily curved region of space can be made
23. Cosmologists realized that galaxies could not have formed just from instabilities in normal matter. The hot
24. Galaxies could then form around the dark-matter clumps, resulting in the Universe we see.
25. A simulation of structure formation in the Universe
26. Clumping of matter in the early Universe would lead to tiny “ripples” in the cosmic background
27. This is a much higher-precision map of the cosmic background radiation. It will likely lead to
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Слайд 2

The Fate of the Universe
Depends on how much mass and energy

there is in the Universe.

Ignoring energy and assuming mass exerts no gravitational pull, the Universe would expand forever at the same rate that it is today (and was in the past).

Слайд 3

The Fate of the Universe
Depends on how much mass and energy

there is in the Universe.

Still ignoring energy but now allowing mass to exert gravitational pull, the Universe would slow down in its expansion (and not get as big).
Gravity acts like friction.

Слайд 4

The Fate of the Universe
Depends on how much mass and energy

there is in the Universe.

If there is enough mass the Universe will collapse back upon itself.

Слайд 5

Comparison to Earth’s Gravity

Слайд 6

The Fate of the Universe
Depends on how much mass and energy

there is in the Universe.

But Dark Energy has a repulsive force that can cause the expansion of the Universe to speed up again.

Слайд 7

The Fate of the Universe
Depends on how much mass and energy

there is in the Universe.

More matter (or less Dark Energy) would could the re-expansion to happen later.

Слайд 8

Possible explanation for the acceleration: vacuum pressure (cosmological constant), more generically

called dark energy.

In reality, the different curves should meet today rather than at the Big Bang. This has important implications for the age of the Universe.

Age of the Universe

Слайд 9

Type I supernovae can be used to measure the behavior of

distant galaxies.
In a decelerating Universe, we expect to see more distant galaxies receeding relatively faster than nearby galaxies.

An Accelerating Universe?

Слайд 10

However, when we look at the data, we see that it

corresponds not to a decelerating universe, but to an accelerating one.
That is, the Universe is dominated by dark energy.

Where we expected the data to be

Where it really is.

Слайд 11

The Critical Density
The amount of mass needed to just barely make

the Universe closed is called the critical density (ρc) (ignoring the effects of dark energy).

Слайд 12

Density and the Fate of the Universe
If Ω > 1, the

Universe will eventually collapse.
If Ω < 1, the Universe will expand forever.
If Ω = 1, the Universe just barely manages to expand forever.

Слайд 13

If the density is low, the universe will expand forever.
If

it is high, the universe will ultimately collapse.

Density

Слайд 14

The answer to this question lies in the actual density of

the Universe.
Measurements of luminous matter suggest that the actual density is only a few percent of the critical density.
But – we know there must be large amounts of dark matter.

Fate of the Cosmos

Слайд 15

However, the best estimates for the amount of dark matter needed

to bind galaxies in clusters, still only bring the observed density up to about 0.3 times the critical density, and it seems very unlikely that there could be enough dark matter to make the density critical.

We can test this by measuring the distances and redshifts of objects.

Слайд 16

Dark Energy and The Cosmological Constant
Curiously, Einstein had introduced this idea

decades before in order to balance gravity and make the Universe “static”.
He later called it the biggest blunder of his career.
Turns out he was right.

Слайд 17

I have drawn these curves starting from the Big Bang, but

we should really draw them as being equal today (as that is all that we really know for sure). This has implications for the age of the Universe.

Age of the Universe

Accelerating Universe

Слайд 18

If space is homogenous, there are three possibilities for its overall

geometry:
Closed – this is the geometry that leads to ultimate collapse
Flat – this corresponds to the critical density
Open – expands forever

Слайд 19

These three possibilities are illustrated here. The closed geometry is like

the surface of a sphere; the flat one is flat; and the open geometry is like a saddle.

The Geometry of Space

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Summary of the Possible Geometries

Слайд 21

Refining the Big Bang Model II: The Flatness Problem
We don’t yet

know the geometry of the Universe, but it appears to be extremely flat.
However, theory says that unless is Ω exactly 1 after the Big Bang, it should be either much smaller or much larger today.
It is unlikely that Ω would have been exactly 1 after the Big Bang.
So, how come the Universe looks so flat today?

Слайд 22

Inflation can also solve the flatness problem.
A heavily curved region of

space can be made to look flat if the radius increases.

Слайд 23

Cosmologists realized that galaxies could not have formed just from instabilities

in normal matter.
The hot radiation from the Big Bang would have kept normal matter from clumping.
But, Dark Matter, being unaffected by radiation, could have started clumping long before normal matter.

Where Did the Galaxies Come From?

Слайд 24