R-squared inflation
E730536
R-squared inflation is a cosmological model of the early universe in which a quadratic term in the curvature of spacetime drives a period of accelerated expansion, providing one of the first successful theories of cosmic inflation.
All labels observed (1)
| Label | Occurrences |
|---|---|
| R-squared inflation canonical | 1 |
Statements (46)
| Predicate | Object |
|---|---|
| instanceOf |
cosmological inflation model
ⓘ
early universe model ⓘ theoretical cosmology model ⓘ |
| addresses |
flatness problem
ⓘ
horizon problem ⓘ monopole problem ⓘ |
| alsoKnownAs | Starobinsky inflation NERFINISHED ⓘ |
| assumes | spatially flat Friedmann–Lemaître–Robertson–Walker metric ⓘ |
| basedOn | modification of Einstein–Hilbert action ⓘ |
| belongsTo | ΛCDM plus inflation paradigm ⓘ |
| category | single-field effective inflation model ⓘ |
| compatibleWith |
Planck satellite data
NERFINISHED
ⓘ
cosmic microwave background observations ⓘ |
| consistentWith | upper bounds on tensor-to-scalar ratio from Planck and BICEP/Keck ⓘ |
| describes | period of accelerated expansion in the early universe ⓘ |
| endsBy | graceful exit via scalaron oscillations ⓘ |
| energyScale | inflation near grand unification scale (order of 10^13 GeV for scalaron mass) ⓘ |
| equivalentTo | single-field slow-roll inflation with scalaron field ⓘ |
| explains | origin of large-scale structure from amplified quantum fluctuations ⓘ |
| feature | inflation driven by gravitational sector rather than matter field ⓘ |
| formulatedIn | 1980 ⓘ |
| framework |
f(R) gravity
ⓘ
modified gravity ⓘ |
| includesTerm |
R^2 term in the gravitational action
ⓘ
quadratic term in the Ricci scalar R ⓘ |
| influenced |
development of f(R) gravity models
ⓘ
subsequent inflationary model building ⓘ |
| introduces | scalaron as effective inflaton ⓘ |
| leadsTo | reheating of the universe after inflation ⓘ |
| mathematicalForm | Einstein–Hilbert action plus R^2 correction term ⓘ |
| namedAfter | Alexei Starobinsky NERFINISHED ⓘ |
| predicts |
Gaussian primordial perturbations to leading order
ⓘ
low level of primordial gravitational waves ⓘ nearly scale-invariant spectrum of scalar perturbations ⓘ quasi–de Sitter expansion in the early universe ⓘ small tensor-to-scalar ratio ⓘ spectral index slightly less than 1 ⓘ |
| proposedBy | Alexei Starobinsky NERFINISHED ⓘ |
| publishedIn | Physics Letters B NERFINISHED ⓘ |
| requires | quantum fluctuations of the scalaron field ⓘ |
| roleInCosmology |
one of the first successful inflationary models
ⓘ
prototype of geometrical inflation ⓘ |
| testedBy |
CMB polarization measurements
ⓘ
CMB temperature anisotropy measurements ⓘ |
| uses |
higher-derivative gravity
ⓘ
slow-roll approximation ⓘ |
Referenced by (1)
Full triples — surface form annotated when it differs from this entity's canonical label.