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Articles: Devotion | Quest for Infinity - 08
- Prof. venkata ramanamurty mallajosyula
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ALEX FRIEDMANN
If Ω has to have a value 1 a long time ago, and we are talking of real small times here, then there is a problem. What is the problem? Simple! Ω equal to 1 means the Universe is flat [see figure in SFI – 02]. Now it is easy to think of the surface of a huge sphere like the present surface as being flat but the surface of a bubble of radius one cm? Can one describe that as being flat? Not really! In which case, how was Ω almost equal to unity a long time ago? This difficulty, by the way, is called the flatness problem.
So there were these two headaches, the horizon problem and the flatness problem that were spoiling the party so to speak. Everybody believed in the Big Bang or wanted to believe in the Big Bang, but if that was true, how to explain away the horizon and the flatness problems? These two knotty issues were got rid of in one masterly stroke by Alan Guth in 1981 via what is now called the Guth’s Inflationary Model.
Guth said: “Look, you guys, let us start with the Universe when it was 10-35 s old. It was very small then; we all agree on that. You know what happened then? I’ll tell you! There was an enormous and astronomical expansion that occurred in the incredibly short time span of 10-32 s. In that time the expansion was all over; and do you know by how much the Universe expanded during that 10-32 s? It expanded 1050 times!” This enormous and sudden expansion is called the Inflation of the Universe.
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