standard model of cosmology




physics, mathematical physics, philosophy of physics

Surveys, textbooks and lecture notes

theory (physics), model (physics)

experiment, measurement, computable physics




The standard model (in theoretical physics) for the observable universe on the largest length scales of cosmology:

it is an inflationary FRW spacetime with cosmological constant (“dark energy”) and cold dark matter. The technical term for this is the Λ\Lambda CDM concordance model (where “Λ\Lambda” is the standard symbol for the cosmological constant and “CDM” is for “cold dark matter”).

The current model assumes that the energy density of the observable universe consists of

(e.g. Einasto 09, fig 17, here)


Vacuum energy and Cosmological constant

The renormalization freedom in perturbative quantization of gravity (perturbative quantum gravity) induces freedom in the choice of vacuum expectation value of the stress-energy tensor and hence in the cosmological constant.

For review see Hack 15, section 3.2.1

For more see at cosmological constant here.

standard model of particle physics and cosmology

gravityelectroweak and strong nuclear forcefermionic matterscalar field
field content:vielbein field eeprincipal connection \nablaspinor ψ\psiscalar field HH
Lagrangian:scalar curvature densityfield strength squaredDirac operator component densityfield strength squared + potential density
L=L = R(e)vol(e)+R(e) vol(e) + F eF +\langle F_\nabla \wedge \star_e F_\nabla\rangle + (ψ,D (e,)ψ)vol(e)+ (\psi , D_{(e,\nabla)} \psi) vol(e) + H¯ eH+(λ|H| 4μ 2|H| 2)vol(e) \nabla \bar H \wedge \star_e \nabla H + \left(\lambda {\vert H\vert}^4 - \mu^2 {\vert H\vert}^2 \right) vol(e)



Lecture notes include

A review is in

  • Jorge L. Cervantes-Cota, George Smoot, Cosmology today – A brief review (2011)(arXiv:1107.1789)

A discussion of open problems is in

See also

In AQFT on Curved spacetimes

Discussion in the rigorous context ofAQFT on curved spacetimes includes

For review see

Last revised on August 3, 2018 at 12:13:20. See the history of this page for a list of all contributions to it.