Peebles–Yu model of photon–baryon fluid
E925296
The Peebles–Yu model of the photon–baryon fluid is a cosmological framework that describes the coupled evolution of photons and baryons in the early universe, providing a basis for understanding the origin of cosmic microwave background anisotropies and acoustic peaks.
All labels observed (1)
| Label | Occurrences |
|---|---|
| Peebles–Yu model of photon–baryon fluid canonical | 1 |
Statements (43)
| Predicate | Object |
|---|---|
| instanceOf |
cosmological model
ⓘ
theoretical framework ⓘ |
| appliesTo | early universe ⓘ |
| assumes |
dominance of radiation over matter at very early times
ⓘ
small perturbations around a homogeneous and isotropic background ⓘ tight-coupling approximation for Thomson scattering ⓘ tightly coupled photons and baryons before recombination ⓘ |
| basedOn | linear perturbation theory ⓘ |
| concerns |
physics of last scattering surface
ⓘ
pre-recombination era ⓘ |
| connectedTo |
standard model of cosmology
ⓘ
ΛCDM cosmology through CMB analysis ⓘ |
| describes |
coupled evolution of photons and baryons
ⓘ
photon–baryon fluid ⓘ |
| developedBy |
J. T. Yu
NERFINISHED
ⓘ
P. J. E. Peebles NERFINISHED ⓘ |
| explains |
acoustic peaks in the cosmic microwave background power spectrum
ⓘ
cosmic microwave background anisotropies ⓘ |
| field |
cosmology
ⓘ
physical cosmology ⓘ |
| frameworkFor |
interpreting CMB temperature power spectrum
ⓘ
linking primordial perturbations to observed CMB features ⓘ |
| historicalSignificance | early quantitative model of CMB anisotropy formation ⓘ |
| includes |
acoustic oscillations of the photon–baryon fluid
ⓘ
baryon inertia effects ⓘ gravitational driving of perturbations ⓘ radiation pressure effects ⓘ |
| incorporates |
damping effects such as Silk damping qualitatively
ⓘ
sound speed of photon–baryon fluid ⓘ |
| influenced | later Boltzmann codes for CMB anisotropy calculations ⓘ |
| predicts |
phase and amplitude of acoustic oscillations
ⓘ
series of acoustic peaks in CMB angular power spectrum ⓘ |
| providesBasisFor |
understanding acoustic oscillations in the photon–baryon fluid
ⓘ
understanding origin of CMB anisotropies ⓘ |
| relatedTo |
baryon acoustic oscillations
ⓘ
cosmic microwave background ⓘ |
| relates |
photon perturbations to gravitational potential perturbations
ⓘ
photon temperature perturbations to density perturbations ⓘ |
| timePeriodOfDevelopment | late 1960s ⓘ |
| treats | photon–baryon mixture as a single fluid on large scales ⓘ |
| usedFor |
estimating positions of CMB acoustic peaks
ⓘ
understanding dependence of peak structure on cosmological parameters ⓘ |
| uses | Friedmann–Robertson–Walker background cosmology NERFINISHED ⓘ |
Referenced by (1)
Full triples — surface form annotated when it differs from this entity's canonical label.