Gibbons–Hawking temperature
E57424
The Gibbons–Hawking temperature is the characteristic thermal radiation temperature associated with the cosmological horizon of de Sitter space, analogous to the Hawking temperature of black holes.
Statements (48)
| Predicate | Object |
|---|---|
| instanceOf |
gravitational phenomenon
ⓘ
physical quantity ⓘ quantum field theory effect ⓘ thermodynamic temperature ⓘ |
| analogousTo |
Hawking radiation
ⓘ
surface form:
Hawking temperature
|
| appearsIn |
semiclassical gravity calculations
ⓘ
studies of de Sitter vacuum structure ⓘ |
| appliesTo |
de Sitter spacetime
ⓘ
surface form:
de Sitter space
spacetimes with cosmological horizon ⓘ |
| associatedWith |
cosmological event horizon
ⓘ
de Sitter spacetime ⓘ
surface form:
de Sitter horizon
vacuum fluctuations in curved spacetime ⓘ |
| characterizes | thermal spectrum seen by inertial observers in de Sitter space ⓘ |
| conceptualRole |
extends black hole thermodynamics to cosmological horizons
ⓘ
links cosmological constant to thermodynamic properties ⓘ |
| consequenceOf |
presence of a cosmological horizon
ⓘ
vacuum state being thermal for static observers ⓘ |
| dependsOn |
k_B
ⓘ
surface form:
Boltzmann constant k_B
Hubble parameter H in de Sitter space ⓘ Planck constant ħ ⓘ cosmological constant Λ ⓘ |
| derivedUsing |
periodicity in imaginary time
ⓘ
quantum field theory on de Sitter background ⓘ |
| describes | thermal radiation of the cosmological horizon ⓘ |
| field |
black hole thermodynamics
ⓘ
cosmology ⓘ general relativity ⓘ quantum field theory in curved spacetime ⓘ |
| hasFormula | T = \frac{\hbar H}{2\pi k_B} ⓘ |
| implies | de Sitter horizon has entropy ⓘ |
| introducedInContextOf |
Euclidean quantum gravity
ⓘ
path integral formulation of gravity ⓘ |
| isNonzeroWhen | cosmological constant is positive ⓘ |
| isZeroWhen | cosmological constant is zero ⓘ |
| namedAfter |
Gary W. Gibbons
ⓘ
Stephen Hawking ⓘ
surface form:
Stephen W. Hawking
|
| observerDependent | yes ⓘ |
| orderOfMagnitudeInOurUniverse | extremely small compared to CMB temperature ⓘ |
| predicts | cosmological horizon emits blackbody radiation ⓘ |
| relatedFormula | T = \frac{\hbar}{2\pi k_B} \sqrt{\frac{\Lambda}{3}} ⓘ |
| relatedTo |
Bekenstein–Hawking entropy
ⓘ
Bekenstein–Hawking entropy ⓘ
surface form:
Gibbons–Hawking entropy
Hawking radiation ⓘ Unruh effect ⓘ |
| relevantFor |
de Sitter phase of the early universe
ⓘ
inflationary cosmology ⓘ late-time de Sitter expansion with dark energy ⓘ |
| unit | kelvin ⓘ |
Referenced by (1)
Full triples — surface form annotated when it differs from this entity's canonical label.