Warm inflation

In physical cosmology, warm inflation is one of two dynamical realizations of cosmological inflation. ^[1]

7 relations: Friedmann equations, General relativity, Graceful exit problem (cosmology), Inflation (cosmology), Physical cosmology, Scale factor (cosmology), Vacuum energy.

Friedmann equations

The Friedmann equations are a set of equations in physical cosmology that govern the expansion of space in homogeneous and isotropic models of the universe within the context of general relativity.

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General relativity (GR, also known as the general theory of relativity or GTR) is the geometric theory of gravitation published by Albert Einstein in 1915 and the current description of gravitation in modern physics.

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Graceful exit problem (cosmology)

The graceful exit problem in cosmology was the need to explain how the universe slowed from its initial inflation to its later rate of expansion.

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Inflation (cosmology)

In physical cosmology, cosmic inflation, cosmological inflation, or just inflation, is a theory of exponential expansion of space in the early universe.

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Physical cosmology

Physical cosmology is the study of the largest-scale structures and dynamics of the Universe and is concerned with fundamental questions about its origin, structure, evolution, and ultimate fate.

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Scale factor (cosmology)

The relative expansion of the universe is parametrized by a dimensionless scale factor a. Also known as the cosmic scale factor or sometimes the Robertson–Walker scale factor, this is a key parameter of the Friedmann equations.

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Vacuum energy

Vacuum energy is an underlying background energy that exists in space throughout the entire Universe.

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References

[1] https://en.wikipedia.org/wiki/Warm_inflation

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