Slides of 5 lectures at XV Brazilian School on Cosmology and ...
Slides of 5 lectures at XV Brazilian School on Cosmology and ...
Slides of 5 lectures at XV Brazilian School on Cosmology and ...
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Dilemma <str<strong>on</strong>g>of</str<strong>on</strong>g> gravit<str<strong>on</strong>g>at</str<strong>on</strong>g>i<strong>on</strong>al energy. . .In GR spacetime carries energy & angular momentumG µν = 8πGc 4 T µνOn account <str<strong>on</strong>g>of</str<strong>on</strong>g> the str<strong>on</strong>g equivalence principle, T µνc<strong>on</strong>tains localizable energy–momentum <strong>on</strong>lyKinetic energy <strong>and</strong> energy associ<str<strong>on</strong>g>at</str<strong>on</strong>g>ed with sp<str<strong>on</strong>g>at</str<strong>on</strong>g>ialcurv<str<strong>on</strong>g>at</str<strong>on</strong>g>ure are in G µν : vari<str<strong>on</strong>g>at</str<strong>on</strong>g>i<strong>on</strong>s are “quasilocal”!Newt<strong>on</strong>ian versi<strong>on</strong>, T − U = −V , <str<strong>on</strong>g>of</str<strong>on</strong>g> Friedmann equ<str<strong>on</strong>g>at</str<strong>on</strong>g>i<strong>on</strong>ȧ 2a 2 + kc2a 2 = 8πGρ3where T = 1 2 mȧ2 x 2 , U = − 1 2 kmc2 x 2 , V = − 4 3 πGρa2 x 2 m;r = a(t)x.15th <str<strong>on</strong>g>Brazilian</str<strong>on</strong>g> <str<strong>on</strong>g>School</str<strong>on</strong>g> <strong>on</strong> <strong>Cosmology</strong> <strong>and</strong> Gravit<str<strong>on</strong>g>at</str<strong>on</strong>g>i<strong>on</strong>, August 2012 – p.13/143
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