13.07.2015 Views

de Sitter space and Holography

de Sitter space and Holography

de Sitter space and Holography

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How to <strong>de</strong>fine conserved charges?The <strong>de</strong>viation of the metric <strong>and</strong> other fields near spatialinfinity from the vacuum provi<strong>de</strong>s a way to <strong>de</strong>fine conservedcharges like mass, angular momentum....Equivalently the conserved charges can be computed fromthe asymptotic symmetries of a <strong>space</strong> time.For example the eigenvalue of an asymptotic timelike Killingvector will give the mass.There are two basic problems to apply this <strong>de</strong>finition for dS<strong>space</strong> (<strong>space</strong>time which is asymptotically dS):1. There is no spatial infinity.2. There is no globally <strong>de</strong>fined asymptotic timelike Killingvector.Fortunately there is a way to proceed generalizing the Brown-York construction to <strong>de</strong>fine stress tensor on the Eucli<strong>de</strong>anboundary <strong>and</strong> by using this quantity to <strong>de</strong>fine mass or othercharges for <strong>space</strong>s which are asymptotically dS.31

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