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SUMMARY:Perturbations and particle creation in non-commutative inflation
DTSTART;VALUE=DATE-TIME:20120504T093000Z
DTEND;VALUE=DATE-TIME:20120504T103000Z
DTSTAMP;VALUE=DATE-TIME:20130522T165516Z
UID:indico-event-189262@cern.ch
DESCRIPTION:We compute the power spectrum of a free scalar field for non-c
 ommutative inflation numerically which is found to be the vacuum spectrum 
 n = 3. Procedure is checked on slow-roll (power-law) inflation and leads t
 o the well-know result n ≃ 1. We discuss two definitions of the classica
 l energy density of a scalar field in a Friedmann universe: The energy obt
 ained from the gravitational energy-momentum tensor and obtained from the 
 canonical energy-momentum tensor of the canonical field Χ= a Φ. We expla
 in the difference in terms of its generating function. Adiabatically renor
 malized energies to order 0\, 2 and 4 are compared analytically and numeri
 cally for slow-roll and non-commutative inflation.\n\nhttp://indico.cern.c
 h/conferenceDisplay.py?confId=189262
LOCATION:Geneva University Room 234
URL:http://indico.cern.ch/conferenceDisplay.py?confId=189262
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