Further astrophysical quantities expected in a quasi-steady state Universe

Details Further astrophysical quantities expected in a quasi-steady state Universe Further astrophysical quantities expected in a quasi-steady state Universe

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...289..729h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 289, no. 3, p. 729-739

Physics

39

Astronomical Models, Cosmology, Dark Matter, Galactic Evolution, Hubble Constant, Mass Distribution, Steady State, Universe, Accretion Disks, Field Theory (Physics), Mass To Light Ratios, Oscillations, Relativistic Theory

Scientific paper

In two previous papers we have described a new cosmological model which we have called the quasi-steady state cosmological model (QSSC) (Hoyle et al. 1993, 1994). In this theory matter is created only in strong gravitational fields associated with dense aggregates of matter. In this paper and in Hoyle et al. (1994) we are attempting to show that many aspects of the observable universe are explicable using this theory so that it is a reasonable alternative to the classical Big-Bang model which has been so widely accepted. We first review briefly the theory of the creation process and show how we arrived at the quasi-oscillatory model. In later sections we show how two of the three parameters of the theory P, and Q, are related to two observed quantities. Q is related to the value of the Hubble constant H0 at the present epoch, and the counts of radio sources enable us to determine P/Q and hence P. We find that Q = 40 x 109 years and P = 8 x 1011 years. We then calculate numerical values for the mass density in the universe and the rate of creation. Finally, we discuss the properties of galaxies including faint galaxies, creation events in individual galaxies, and the mass-to-light ratios in galaxies and clusters. The results here are particularly interesting since in this model stars can be much older than 1/H0. This means that much of the mass in galaxies will naturally be baryonic and will consist of evolved stars. Thus very large mass-to-light ratios are expected in galaxies and in clusters. We conclude by summarizing the results obtained in all three papers. More work is required, particularly on the cosmogonical aspects of the theory, but a very attractive aspect of it is that the creation process in the centers of galaxies leads to a comparatively simple way of understanding explosive phenomena.

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