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Liang Dai1, Marc Kamionkowski1, Junpu Wang1

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Reheating after inflation imposes new constraints on inflationary models. Chaotic inflation (α=2) is compatible with standard reheating, while other models require exotic conditions or specific scalar spectral index values for consistency.

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Area of Science:

  • Cosmology and astrophysics
  • Theoretical physics
  • Particle physics

Background:

  • BICEP2 experiment detected a significant gravitational-wave background, favoring inflaton potentials like V(ϕ)∝ϕ^α.
  • Chaotic inflation (α=2) and axion-monodromy models are of particular interest.
  • The reheating phase, connecting inflation to the radiation era, is crucial for model constraints.

Purpose of the Study:

  • To investigate how reheating considerations constrain inflationary models, specifically V(ϕ)∝ϕ^α.
  • To analyze the impact of the effective equation-of-state parameter during reheating (w(re)) on different α values.
  • To establish relationships between reheat temperature (T(re)) and scalar spectral index (n(s)) for specific models.

Main Methods:

  • Modeling the reheating phase using an effective equation-of-state parameter, w(re).
  • Analyzing consistency between different inflationary potentials (α=1, 2, 4, 2/3) and reheating scenarios (w(re)=0 or -1/3 < w(re) < 0).
  • Deriving a quantitative relation between T(re) and n(s) for the m(2)ϕ(2) inflation model with canonical reheating.

Main Results:

  • α=2 models are consistent with canonical reheating (w(re)=0) for n(s) within the 1σ range.
  • Models with α=1 or α=2/3 require exotic reheating (-1/3 < w(re) < 0) unless n(s) is higher.
  • α=4 models necessitate implausible reheating (w(re) > 1/3) unless n(s) is near the 2σ lower limit.

Conclusions:

  • Reheating constraints can distinguish between various inflationary models, including chaotic and axion-monodromy.
  • The derived relation for m(2)ϕ(2) inflation suggests T(re) ≲ 10^6 GeV if n(s) is near its central value.
  • Future precise measurements of n(s) will be key to testing these models and the m(2)ϕ(2) prediction of n(s) ≃ 0.965.