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Flatness ProblemThe Universe has total Omega = 1. Is this a problem? Yes. To understand this point, recall that the Universe is fairly old, 13.7 billion years and that Omega = 1 is for a critical Universe. Analogy: Try and balance a pencil on its pointed end. If you are far from vertical, the pencil falls to the ground very quickly. The closer you can place the pencil to vertical the longer it stands-up before it falls over. If you could place it at precisely vertical then (classically) it could stand-up forever. It is hard to place the pencil at its critcal position. Universe: If the Universe started off far from critical, then it would have either quickly collapsed (not lasted for 13.7 billion years) or it would have expanded so quickly that it would have passed through the nucleosynthesis and galaxy formation epochs so fast that we would not be here. The only way for the Universe to have lasted this long and to have passed through the nucleosynthesis era at leisurely enough rates requires that the Universe started off very close to critical. How close? Amazingly,
to make Omega(t) ~ 1 today. This is Flatness Problem. |
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The above mysteries may be explained by what is known as the Inflation Theory . Recently results from the Wilkinson Microwave Anisotropy Probe (WMAP) offered strong support for the Inflation theory. To get a handle on inflation recall that the nature of the four forces of nature changes as the Universe evolves:
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The end of the GUT era is signaled by the symmetry breaking where the nuclear (strong) and electro-weak forces become distinct forces. This is the event where inflation is driven.
The symmetry breakings are analogous to
phase transitions (e.g., liquid water ---> solid water (ice),
liquid water ---> vapor, etc.). Similarly to the phenomenom of
supercooling (Youtube video), the phase transition can be delayed,
(and, as for water) the energy difference between the phases
abruptly released at the end of the transition
freezing water produces heat (Youtube video). The phase transition
at the end of the GUT era behaves in this manner.
Inflation may be driven by a nonzero Cosmological Constant
; ah ha, there might be
one even in the early Universe,
but the Cosmological Constant
must be reasonably small (fine-tuning) and it must essentially disappear or
decay (or
become very small) as the Universe evolves.
During inflation, the scale factor of the Universe
R(t) evolves as:
In the example, the Universe grows by a factor of more than 1030
in 10-32 sec. The exact rate at which the Universe grows depends
on the particular model. The point is that the expansion rate is humongous!
(Note that in this example, the Universe expands so quickly
that even a light beam
emitted from a distant observer cannot reach the Earth; the amount of
ground it has to cover grows too fast. We say that the
horizon of the observer actually gets smaller in the sense that we see less
of the Universe as time passes!)
This explains the horizon problem.
Inflation predicts that the Universe should appear flat
(that is, Omega = 1, identically). This resolves the
flatness problem.
What are some consequences of this blow-up?
Suppose that we start with a large universe and consider a small causally
connected chunk say, of size 10-24 cm. Suppose the Universe
inflates and that inflation lasts for 10-32 sec,
The causally connected chunk of the
Universe expands to a size 10 km. This
inflated patch easily encompasses our Universe which, at this time, is
only ~ 30 cm in size. Our Universe was embedded in this huge
region which was causally connected before inflation,
The Earth is known to be spherical, however,
for us small (short people) living on
the surface of the Earth, the Earth appears flat. It appears flat because we are
not tall enough to see over the edge of the Earth.
Due to inflation, we have
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