lecture18

lecture18 - Early Universe hotter, more energetic and...

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Early Universe hotter, more energetic and denser high energy radiation ( γ rays) dominated matter nuclei destroyed, would not exist pair creation from high-E γ rays uniFcation of forces Today -- follow this evolution as the universe expands cools and lowers it’s density
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As universe expands, T/energy is major determinant : Pair creation : matter energy/photons eg. γ + γ p + + p - requires E 2 γ = 2 m p c 2 2x938 Mev >10 13 K γ + γ e - + e + requires E 2 γ = 2 m e c 2 2x511 kev >6x10 9 K Unifcation oF Forces : m w,z ~ 90 Gev , above 10 15 K γ + γ w,w * z,z * ( γ ’s are EM) unifed electro-weak Force strong nuclear Force 10 19 Gev 10 32 K expect unifcation oF nuclear & E Force
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Four forces in physics :
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age physical event T <10 -44 sec > 10 32 K 10 -44 sec Quantum gravity -- all 4 Forces unifed 10 32 K 10 -35 sec
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This note was uploaded on 09/25/2010 for the course AY 106 taught by Professor Schrerr during the Winter '09 term at UMBC.

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lecture18 - Early Universe hotter, more energetic and...

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