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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.
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!)
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This explains the horizon problem.
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Inflation predicts that the Universe should appear flat (that is, Omega = 1, identically). This resolves the flatness problem.
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