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Natural inflation: Particle physics models, power law spectra for large scale structure, and constraints from COBE

Jun, 1992
55 pages
Published in:
  • Phys.Rev.D 47 (1993) 426-455
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DOI:
Report number:
  • FERMILAB-PUB-92-202-A
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Abstract:
A pseudo-Nambu-Goldstone boson, with a potential of the form V(ϕ)=Λ 4[1±cos⁡(ϕ/f)],naturallygivesrisetoinflationifV(\phi) = \Lambda~4[1 \pm \cos(\phi/f)], naturally gives rise to inflation if f \sim M_{Pl}and and \Lambda \sim M_{GUT}.Weshowhowthiscanariseintechnicolor−likeandsuperstringmodels,andworkoutanexplicitstringexampleinthecontextofmultiplegauginocondensationmodels.Westudythecosmologyofthismodelindetail,andfindthatsufficientreheatingtoensurethatbaryogenesiscantakeplacerequires. We show how this can arise in technicolor-like and superstring models, and work out an explicit string example in the context of multiple gaugino condensation models. We study the cosmology of this model in detail, and find that sufficient reheating to ensure that baryogenesis can take place requires f > 0.3 M_{Pl}.Theprimordialdensityfluctuationspectrumgeneratedisanon−scale−invariantpowerlaw,. The primordial density fluctuation spectrum generated is a non-scale-invariant power law, P(k) \propto k~{n_s},with, with n_s \simeq 1 - (M~2_{Pl}/8\pi f~2),leadingtomorepoweronlargelengthscalesthanthe, leading to more power on large length scales than the n_s = 1Harrison−Zeldovichspectrum.ThestandardCDMmodelwith Harrison-Zeldovich spectrum. The standard CDM model with 0 \la n_s \la 0.6-0.7couldinprincipleexplainthelarge−scaleclusteringobservedintheAPMandIRASgalaxysurveysaswellaslarge−scaleflows,buttheCOBEmicrowaveanisotropyimpliessuchlowamplitudes(orhighbiasfactors, could in principle explain the large-scale clustering observed in the APM and IRAS galaxy surveys as well as large-scale flows, but the COBE microwave anisotropy implies such low amplitudes (or high bias factors, b>2)fortheseCDMmodelsthatgalaxyformationoccurstoolatetobeviable;combiningCOBEwithsufficientlyearlygalaxyformationorthelarge−scaleflowsleadsto) for these CDM models that galaxy formation occurs too late to be viable; combining COBE with sufficiently early galaxy formation or the large-scale flows leads to n_s >0.6,or, or f > 0.3 M_{Pl}aswell.Forextendedandpowerlawinflationmodels,thisconstraintiseventighter, as well. For extended and power law inflation models, this constraint is even tighter, n_s > 0.7$; combined with other bounds on large bubbles in extended inflation, this leaves little room for most extended models.
  • inflation
  • particle physics
  • Goldstone particle
  • string model
  • supergravity
  • gaugino: condensation
  • galaxy
  • dark matter
  • cosmic radiation: anisotropy
  • symmetry breaking
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