Compare · The Origin of Our Universe

Warm Inflation vs New Inflation

Inflationary Big Bang· within family

	Warm Inflation Strongly supported	New Inflation Historical
Proposed	1995 / 2020	1982
Key figures	Arjun Berera, Ian Moss, Rudnei Ramos, Mar Bastero-Gil	Andrei Linde, Andreas Albrecht, Paul Steinhardt
In one sentence	Warm inflation adds friction to the inflaton field: it transfers energy into a radiation bath as it rolls, so the universe stays hot during inflation and slides straight into the radiation era with no distinct reheating phase.	Linde and independently Albrecht and Steinhardt replaced Old Inflation's bubble nucleation with a scalar field slowly rolling down a flat potential, producing a coherent end to inflation across whole Hubble regions and the first viable predictions for cosmological perturbations.
Predictions	A radiation bath persists throughout inflation, so the handover to the hot Big Bang is smooth, with no separate reheating phase. Density perturbations are sourced largely by thermal fluctuations rather than vacuum fluctuations, which raises the scalar amplitude and lowers the tensor-to-scalar ratio relative to cold inflation on the same potential. A distinct non-Gaussian signature in the primordial perturbations, different in shape and sign from the small non-Gaussianity of cold single-field inflation. Viable inflation on steeper potentials than cold inflation allows, easing the flatness fine-tuning and the tension with swampland-type conjectures.	Nearly scale-invariant spectrum of primordial density perturbations with scalar spectral index slightly less than 1 Approximately Gaussian, adiabatic primordial fluctuations Small but nonzero gravitational wave background depending on the potential shape
Where it breaks	Deriving the dissipation strength from first-principles quantum field theory is hard: the inflaton must couple strongly enough to thermalize a bath, yet not so strongly that radiative corrections spoil the potential's flatness. Thermal backreaction can destabilize the slow roll, and many early warm-inflation models did not survive a careful treatment of it. Current cosmological data do not require warm inflation over cold inflation. It is a viable alternative, not a preferred one, and its sharpest signature, the non-Gaussian shape, sits below present detection thresholds.	Requires the inflaton to start very near the top of a flat potential, which is a finely tuned initial state. Realizing sufficiently flat small-field potentials compatible with particle physics is difficult; quantum corrections tend to spoil the required flatness. Specific potentials of this class are now disfavored or ruled out by Planck data, even though the slow-roll mechanism itself remains the working framework.
Key unresolved problem	The dissipation coefficient problem: it is hard to calculate the friction from basic quantum field theory, because coupling the field strongly enough to heat up a radiation bath tends to wrinkle the flat potential the model relies on.	The flatness fine-tuning problem: the model needs an exceptionally flat potential for the field to roll down, but quantum corrections from particle physics tend to wrinkle that potential and ruin the flatness it depends on.
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Warm Inflation

1995 / 2020 · Strongly supported

New Inflation

1982 · Historical

Proposed

1995 / 2020

1982

Key figures

Arjun Berera, Ian Moss, Rudnei Ramos, Mar Bastero-Gil

Andrei Linde, Andreas Albrecht, Paul Steinhardt

In one sentence

Warm inflation adds friction to the inflaton field: it transfers energy into a radiation bath as it rolls, so the universe stays hot during inflation and slides straight into the radiation era with no distinct reheating phase.

Linde and independently Albrecht and Steinhardt replaced Old Inflation's bubble nucleation with a scalar field slowly rolling down a flat potential, producing a coherent end to inflation across whole Hubble regions and the first viable predictions for cosmological perturbations.

Predictions

A radiation bath persists throughout inflation, so the handover to the hot Big Bang is smooth, with no separate reheating phase.
Density perturbations are sourced largely by thermal fluctuations rather than vacuum fluctuations, which raises the scalar amplitude and lowers the tensor-to-scalar ratio relative to cold inflation on the same potential.
A distinct non-Gaussian signature in the primordial perturbations, different in shape and sign from the small non-Gaussianity of cold single-field inflation.
Viable inflation on steeper potentials than cold inflation allows, easing the flatness fine-tuning and the tension with swampland-type conjectures.

Nearly scale-invariant spectrum of primordial density perturbations with scalar spectral index slightly less than 1
Approximately Gaussian, adiabatic primordial fluctuations
Small but nonzero gravitational wave background depending on the potential shape

Where it breaks

Deriving the dissipation strength from first-principles quantum field theory is hard: the inflaton must couple strongly enough to thermalize a bath, yet not so strongly that radiative corrections spoil the potential's flatness.
Thermal backreaction can destabilize the slow roll, and many early warm-inflation models did not survive a careful treatment of it.
Current cosmological data do not require warm inflation over cold inflation. It is a viable alternative, not a preferred one, and its sharpest signature, the non-Gaussian shape, sits below present detection thresholds.

Requires the inflaton to start very near the top of a flat potential, which is a finely tuned initial state.
Realizing sufficiently flat small-field potentials compatible with particle physics is difficult; quantum corrections tend to spoil the required flatness.
Specific potentials of this class are now disfavored or ruled out by Planck data, even though the slow-roll mechanism itself remains the working framework.

Key unresolved problem

The dissipation coefficient problem: it is hard to calculate the friction from basic quantum field theory, because coupling the field strongly enough to heat up a radiation bath tends to wrinkle the flat potential the model relies on.

The flatness fine-tuning problem: the model needs an exceptionally flat potential for the field to roll down, but quantum corrections from particle physics tend to wrinkle that potential and ruin the flatness it depends on.

Reader vote

No votes yet