High order correlation functions for a self-interacting scalar field in de Sitter space

Physical Review D - Particles, Fields, Gravitation and Cosmology

Volumn 69, Issue 6, 2004, Pages 6-

  Bernardeau, Francis ^a   Brunier, Tristan ^a   Uzan, Jean Philippe ^b,c  

^a CEA SACLAY   (France)

^b UNIVERSITÉ PARIS SUD   (France)

^c INSTITUT D'ASTROPHYSIQUE DE PARIS   (France)

Author keywords

[No Author keywords available]

Indexed keywords

EID: 2342417637     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.69.063520     Document Type: Article

References (18)

1. A. Guth Phys. Rev. D 23, 347 (1981).
2. D.N. Spergel, Astrophys. J., Suppl. 148, 175 (2003)
3. Astrophys. J., Suppl.H.V. Peiris, 148, 213 (2003).
4. S. Mukhanov and G.V. Chibisov, Pis’ma Zh. Éksp. Teor. Fiz. 33, 549 (1981) [JETP Lett. 33, 532 (1981)]
5. S.W. Hawking, Phys. Lett. 115B, 295 (1982)
6. V.F. Mukhanov, H.A. Feldman, and R.H. Brandenberger, Phys. Rep. 215, 203 (1992);A.D. Linde, Particle Physics and Inflationary Cosmology (Harwood, Chur, Switzerland, 1990);A.R. Liddle and D.H. Lyth, Cosmological Inflation and Large-Scale Structure (Cambridge University Press, Cambridge, 2000).
7. J. Maldecena, J. High Energy Phys. 0305, 013 (2003).
8. P. Creminelli, J. Cosmol. Astropart. Phys. 10, 003 (2003).
9. N. Bartolo, S. Matarrese, and A. Riotto, Phys. Rev. D 64, 083514 (2001).
10. N. Bartolo, S. Matarrese, and A. Riotto, Phys. Rev. D 65, 103505 (2002).
11. F. Bernardeau and J.-P. Uzan, Phys. Rev. D 66, 103506 (2002).
12. F. Bernardeau and J.-P. Uzan, Phys. Rev. D 67, 121301(R) (2003).
13. S. Hawking and G.F.R. Ellis, Large Scales Structure of Spacetime (Cambridge University Press, Cambridge, 1973).
14. N.D. Birrel and P.C.W. Davies, Quantum Fields in Curved Space (Cambridge University Press, Cambridge, 1982).
15. N.C. Tsamis and R.D. Woodard, Class. Quantum Grav. 11, 2969 (1994).
16. F. Bernardeau and J.-P. Uzan, astro-ph/0311421.
17. Calculations in other backgrounds are difficult in general but we have checked that in case of a power law inflation, (Formula presented) we recover the same behaviors in the superhorizon limit if (Formula presented) is large enough.
18. It is to be noted that these calculations do not correspond to those of diffusion amplitudes of some interaction processes in a de Sitter space. When one tries to do these latter calculations with a path integral formulations, mathematical divergences are encountered as it has been stressed in Refs. 812. With that respect de Sitter space differs from Minkowski space-time. Our current point of view on this difficulty is that diffusion amplitudes cannot be properly defined in de Sitter space and that only field correlators as defined here correspond to actual observable quantities that can be safely computed.