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Natural Inflation: Particle Physics Models, Power Law Spectra for Large Scale Structure, and Constraints from COBE
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abstract
A pseudo-Nambu-Goldstone boson, with a potential of the form $V(\phi) = \Lambda^4[1 \pm \cos(\phi/f)], naturally gives rise to inflation if $f \sim M_{Pl}$ and $\Lambda \sim M_{GUT}$. 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 $f > 0.3 M_{Pl}$. The primordial density fluctuation spectrum generated is a non-scale-invariant power law, $P(k) \propto k^{n_s}$, with $n_s \simeq 1 - (M^2_{Pl}/8\pi f^2)$, leading to more power on large length scales than the $n_s = 1$ Harrison-Zeldovich spectrum. The standard CDM model with $0 \la n_s \la 0.6-0.7$ 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, $b>2$) 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 $f > 0.3 M_{Pl}$ 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.
Forward citations
Cited by 11 Pith papers
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Extra-dimensional Origins of Chemical Potentials at the Cosmological Collider
A rolling 5D gauge-field inflaton acts as an extra-dimensional electric field, creating charged and neutral KK particles far heavier than H and yielding observable oscillatory signatures.
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Kinetic Gauge Friction in Natural Inflation
Kinetic gauge friction can sustain natural inflation with sub-Planckian f, and a Chern-Simons term stabilizes the perturbations, yielding CMB-compatible spectra.
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Galaxy Clusters Selected via the Sunyaev-Zel'dovich Effect in 5 year data from the SPT-3G Main Survey
A catalog of 7190 confirmed galaxy clusters from 5-year SPT-3G SZ observations spanning masses 7.9e13 to 1.6e15 solar masses and redshifts 0.037 to >2.
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Post-inflationary enhancement of adiabatic perturbations in modular cosmology
In modular inflation models, entropic perturbations frozen during inflation are converted into curvature perturbations after inflation, producing an enhanced power spectrum while preserving the spectral index ns.
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Axion USR Inflation
In axion inflation with an intermediate ultra-slow-roll phase, the instability parameter collapses at the start of USR, terminating gauge production and yielding a two-peak power spectrum with P_R ∝ k^m, m>4.
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Pure Chromo-Natural Inflation: Signatures of Particle Production from Weak to Strong Backreaction
Pure chromo-natural inflation unavoidably transitions from weak to strong backreaction, producing a chiral three-peak gravitational wave spectrum and a scalar peak that can form primordial black holes.
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Corrections to inflationary models induced by non-minimal coupling between scalar field and curvature
Power-law non-minimal coupling F=(H/λ)^{2n} deforms inflationary potentials, shifts r and n_S while preserving n_T=-r/8 and GR-like reheating, enabling r(1-n_S) classification of models against Planck/ACT data.
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Comparative study of the strong backreaction regime in axion inflation: the effect of the potential
In lattice simulations of axion inflation, the strong-backreaction stage that lengthens inflation occurs for all seven tested potentials, but its duration varies strongly with the potential.
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QCD Axion on Hilltop by a Phase Shift of $\pi$
A heavy axion inflaton can shift the QCD axion potential by π, placing the QCD axion at the hilltop and allowing f_a ≳ 3×10^9 GeV to explain all dark matter.
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A multi-axion model of inflation and dark matter
A 300-mode Kaluza-Klein axion tower is proposed as a unified inflaton and dark-matter sector, but the lightest state's quoted lifetime contradicts the paper's own decay-rate formula.
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Axions as Dark Matter, Dark Energy, and Dark Radiation
A mini-review of axion phenomenology showing how light bosons can account for dark matter, drive cosmic acceleration, or contribute to relativistic backgrounds in the early and late Universe.
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