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SUMMARY:How Many Angels Can Sit on the Head of a Black Hole
DTSTART;VALUE=DATE-TIME:20170314T090000Z
DTEND;VALUE=DATE-TIME:20170314T100000Z
DTSTAMP;VALUE=DATE-TIME:20180222T185710Z
UID:indico-event-5558@cern.ch
DESCRIPTION:The fundamental work of Bekenstein and Hawking on the thermody
namics of black holes gives us clues to a general theory of quantum gravit
y. The most important of these is the Covariant Entropy Principle\, which
links Geometry and Quantum Mechanics: the logarithm of the dimension of t
he Hilbert space describing physics in a causal diamond in any space-time
is equal\, in the limit of large area\, to one quarter of the maximal spac
e-like area on the boundary of the diamond\, measured in Planck units. Thi
s holds\, in particular\, for de Sitter space\, which is the space-time ou
r own universe will approach in the asymptotic future. In that case the t
otal dimension is finite. It was proposed by 't Hooft that all of the degr
ees of freedom describing a causal diamond live on that maximal area surfa
ce\, and by Fischler and myself that excitations localized in the interior
of the diamond correspond to constrained states of these boundary degrees
of freedom. The latter principle has profound implications for early uni
verse cosmology and for the theory of supersymmetry breaking. It leads to
a mathematically finite theory of inflation and predicts the existence of
supersymmetric partner particles in the multi TeV regime\, possibly acces
sible to the LHC.\n\nhttps://indico.tifr.res.in/indico/conferenceDisplay.p
y?confId=5558
LOCATION: AG80
URL:https://indico.tifr.res.in/indico/conferenceDisplay.py?confId=5558
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