Other
Scientific paper
Feb 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975gregr...6....9b&link_type=abstract
General Relativity and Gravitation, Volume 6, Issue 1, pp.9-12
Other
Scientific paper
It is sometimes said that, if the universe were not expanding, we all would burn up, (Olbers' paradox). In order to check on this, I have used a solution of Friedmann's equation that seems reasonable, and that predicts a contraction of the universe after it has reached a maximum size. We may then compare the radiation energy density U n now at age t n of the universe, with this density (=U * ) at a time t * during contraction when R(t) takes a value R * equal to its present value R n .We simplify the calculation by choosing 2R n as maximum of R(t). Then, t n=(1/2 π-1)R n/C=6.98 × 109 year for R n = 1.16× 1028 cm.(The present density would then be ρn = 2.4× 10-29 gram/cm3).We assume the number of galaxies per unit volume = N(t) = η/R(t) 3 with constant η,and we assume a constant average radiative power L per galaxy. Now at t n we choose N n L ≈ 10-31 erg/cm3sec,but our conclusions would be the same for much larger values of this. We split U into three parts: U 1 is the primordial energy density left over from t ≈ 0.We put U 1(t n ) ≈ 6× 10-13 erg/cm3 corresponding to T ≈ 3°K.U 2 is the density of the energy flux near the earth emitted by all stars in our own Milky Way. Most of it is the density U S =L &sun;/4ηr 2 c = 4.5 × 10-5 erg/cm3 in the flux from the sun. Finally, U 3 is the energy in the radiation emitted by all other galaxies since t ≈ 0, and was going to burn us according to Olbers. Since U 1 is a function of R(t), we put U 1(t*) =U 1 (t n ).We shall also assume U 2 to be unchanged, as it was not the effect of a change of U s that we were investigating. In calculating U 3 we shall overestimate it by neglecting the absorption by closer galaxies of some of the light emitted by farther ones.
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