Slow rotational perturbations of Friedmann universes

Details Slow rotational perturbations of Friedmann universes Slow rotational perturbations of Friedmann universes

May 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990ap%26ss.167..341y&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 167, no. 2, May 1990, p. 341-345.

Astronomy and Astrophysics

Astrophysics

1

Cosmology, Galactic Evolution, Missing Mass (Astrophysics), Perturbation Theory, Universe, Angular Velocity, Coordinate Transformations, Einstein Equations

Scientific paper

Exact solutions of the field equations belonging to the perturbed metric in the case of perfect fluid are examined, and a comparison with approximate solutions by other authors is made. In the general case, where all the terms are included, the field equations are shown to give Omega = Omega(t). In this case, since the condition Omega = 0 can be accomplished by a coordinate transformation, the solutions of field equations reduce to those of the classical Friedmann equations; and approximate solutions become formal solutions without physical interest.

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