ARlogo Annu. Rev. Astron. Astrophys. 1991. 29: 325-362
Copyright © 1991 by Annual Reviews. All rights reserved

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3.3 Historical Comment

We have already pointed out the similarity between the inflationary phase and the de Sitter spacetime. A closer similarity exists between some of the ideas invoked in inflation and the steady state model (16, 55). In the steady state model, a steady exponential expansion [with (adot / a) = constant] was made compatible with a constant density of matter (rho = constant) by invoking the continuous creation of matter. Where did this matter come from?

McCrea (78) had proposed negative stresses in vacuum to provide the required energy tensor to drive the expansion. In the 1950s, particle physics had not advanced to the sophisticated levels of today and so McCrea's phenomenological ideas were largely ignored by physicists. Today we can view them with greater sympathy.

An alternative theory based on Hoyle's earlier ideas of a cosmological field creating matter (55, 56) was investigated further by Hoyle & Narlikar (57, 58, 59, 60). This involved a scalar C-field, whose action function was first proposed by Pryce (103; private communication). The C-field action had two terms as part of the overall Hilbert action:

Equation 29a
Equation 29b 29.

of which the first, pure field term had a negative energy density and negative stresses for the coupling constant f > 0. This was responsible for driving the expansion. The second, field-matter interaction term, involving the effect of the C-field on matter particles (labelled by a, b, . . .) and vice versa, came into operation only at the instant of creation of matter.

The advantage of the formulation by Pryce was that it is based on an action principle and hence guarantees conservation of matter and energy. In the steady state solution, matter creation is compensated by augmentation of the strength of the C-field, which has negative energy. In this solution the Hubble constant is given by

Equation 30 30.

There were also solutions of this theory with no creation of matter, however. What role did they have to play? Hoyle & Narlikar (59) argued that these solutions appear as ``bubbles'' in a highly dense steady state universe with H >> H0, the present value of Hubble's constant. The mechanism of the switch-over from a ``creation'' to ``noncreation'' mode was left undiscussed for want of a quantum field theory of the C-field.

Thus, the key idea of the inflationary scenario of the present FRW model originating as a bubble in an external de Sitter type universe was anticipated 15 years earlier. The 1966 version [like McCrea's (78) 1951 paper] appeared too far ahead of its time to be appreciated by the contemporary particle physicists.

Finally, the cosmic baldness conjecture had also been anticipated by the steady state cosmology (57), which argued that the C-field driven expansion would wipe away any initial departures from nonuniformity.

In later years, other papers discussed the idea of inflation before or around the time of Guth's paper. For example, Kazanas (67) explicitly discussed the notion of inflation as a solution to the horizon problem. Kazanas assumed a temperature-dependent energy density of the vacuum and showed that during the phase transition, the universe would expand substantially faster than the a propto t1/2 law. For some temperature-dependent vacuum energies Kazanas obtained an exponential expansion law.

Sato (107) also discussed the implications of a first order phase transition of vacuum in the very early universe, and obtained the exponential expansion rate. Sato calculated the bubble nucleation rate, which depends on the particle physics theory used. He found that if the nucleation rates are small and the vacuum stays at the metastable state for a long enough time, the universe would expand exponentially, with the result that the phase transition would be further stretched out in time. Sato also considered the possibility of density and velocity fluctuations created by the phase transition growing to form galaxies.

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