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Articles: Devotion | Quest for Infinity - 08
- Prof. venkata ramanamurty mallajosyula
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The inflationary model of Guth solves this by saying the following. At time t = 10-35 s, the radius of the Universe was very small, so small that radiation everywhere could freely mix, making uniformity possible all across the Universe. At that instant, the Universe suddenly “blows up’ or inflates enormously. The radius now becomes 1 cm, and thereafter, radiation mixing is not possible; but no problem, since equilibrium has already been established and that status quo is just maintained! Clever, is it not? But the beauty is that this daring conjecture has actually been substantiated by experiments!
What I have outlined above may be called problem number one; it is called the horizon problem [for reasons we need not go into here]. There is one more problem, problem number two, which I shall now describe briefly. To explain this problem, I would first have to recall what I said earlier [see SFI – 02] about the three possible scenarios concerning the expansion history of the Universe. I pointed out in that instalment that Alexander Friedmann in Russia figured out three possible ways in which the Universe can evolve, these three scenarios being decided by the value of a parameter called Omega Ω.
Searching for the Value of Omega Ω
Current studies suggest that Ω is close to unity. Fine, so it is, and that is the way God has decided it should be. However, this value of 1 for Ω creates a headache for cosmologists. According to them, if Ω is almost 1 now, it must have been that way a long time also [there are strong technical reasons for so arguing but those I have to skip].
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