A cosmological mode is on a superhorizon scale when its physical wavenumber is smaller than the Hubble expansion rate, k/a≪H, equivalently k≪aH.
Ancestors (11)
- Cosmological horizon exit
- Bunch-Davies vacuum
- Canonically rescaled de Sitter scalar mode
- Inflationary scalar Fourier mode
- Inflaton action in an expanding universe
- Inflaton
- Cosmic inflation
- Cosmology
- Branches of physics
- Physics
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Incoming links (32)
- Adiabatic initial conditions
- Adiabatic matter-string density relation
- CDM density equation in a matter-radiation universe
- Conformal-time quadratic action for an inflaton perturbation
- Cosmological horizon entry
- Equal-time two-point function of a de Sitter scalar
- Frozen contribution to a de Sitter scalar spectrum
- Matter-era density transfer from primordial curvature
- Non-adiabatic pressure perturbation
- Past exam of the mathematics course of the University of Cambridge / 2001 / iii / Paper 67 / 4 / iii / Solution
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- Past exam of the mathematics course of the University of Cambridge / 2016 / iii / Paper 310 / 2 / c / Solution
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- Radiation-era adiabatic potentials with free-streaming neutrinos
- Superhorizon conservation of uniform-density curvature
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