Browsing by Author "Hoyle, F."

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Astrophysical deductions from the quasi-steady state cosmology
(Wiley-Blackwell, 1993-11-24) Hoyle, F.; Burbidge, G.; Narlikar, J. V.
The numerical consequences of the theory developed in two previous papers are examined in more detail. In particular, it is shown that the radio source count data can be explained to high accuracy, including the steeper-than-Euclidean slope of the count distribution at its high-flux end. By specifying the parameters of the theory, we obtain reasonable values for the Hubble constant and the ages of the globular clusters, a maximum redshift for any object observed from the present oscillatory cycle of the Universe, a minimum average density of ˜2 × 10¯²7 g cm¯³ for clusters of galaxies, and a temperature close to 2.7 K for the microwave background. The theory predicts a near-blackbody spectrum for the microwave background, and also explains the observed anisotropy.
Basic theory underlying the quasi-steady state cosmology
(Royal Society Publishing, 1995-02-08) Hoyle, F.; Burbidge, G.; Narlikar, J. V.
Outside cosmology, the procedure normally followed in science requires the inte- gration of hyperbolic partial differential equations subject to initial data given on a free surface, which is usually taken to be a time section of spacetime. The initial data are determined in experimental science from observation and the re- sults of the integrations are also checked by observations. Friedmann (Big Bang) cosmology suffers, however, from the fact that the observations cannot determine initial conditions. Thus in that theory the initial conditions have only the weak status of guesses. There is also some question whether the correct equations are being used, since the gravitational equations of that cosmology are not scale invariant, a situation unlike the rest of physics. Since matter exists in what is supposed to be a space of finite temporal duration its origin should be explained, working from a suitable lagrangian and action. Otherwise the origin is placed outside science. This is what is done in Big Bang cosmology. In this paper we depart from the standard procedure by first deriving grav- itational equations that are scale invariant, whence it is shown that in a scale invariant gravitational theory particles have the property that the two lengths associated with them, the Compton wavelength and gravitational radius, must be comparable, i.e. they are Planck particles. It is then shown that the theory has the scope to explain the genesis of the so-called cosmological constant, and the usually required magnitude of the cosmological constant is derived. When interactions other than gravitation are included, Planck particles are un- stable. The effect of instability on newly created Planck particles is to introduce terms into the gravitational equations additional to those of general relativity. In particular, there are negative pressure terms which act to expand the universe. The energy terms are such as to suggest that particle creation must be of an ex- plosive nature and that it must occur in the neighbourhoods of highly compacted bodies, a property which appears to provide a connection between cosmological theory and high-energy astrophysics.
C-field as a direct particle field
(Royal Society, 1964-11-03) Hoyle, F.; Narlikar, J. V.
It has been known for some years that a C-field, generated by a certain source equation, leads to interesting changes in the cosmological solutions of Einstein's equations. The steady- state cosmology appears as an asymptotic case. The source equation has so far only been given in the macroscopic case of a smooth fluid. In the present paper we derive the source equation in terms of discrete particles. The method adopted is similar to that we have recently given for the generalization to Riemannian space of the Fokker action principle in the electro- magnetic theory. In the latter, a 4-vector is defined in terms of the world lines of particles. The definition is such that the four-dimensional curl of the vector satisfies Maxwell's equations, which are therefore identities. Similarly, C is a scalar defined in terms of the world-lines of particles, and the source equation used formerly then follows as an identity.
Conformal invariance in physics and cosmology
(Colorado Associated University Press, 1972-01-10) Hoyle, F.; Narlikar, J. V.
Conformal theory of gravitation
(Royal Society, 1966-09-20) Hoyle, F.; Narlikar, J. V.
Certaini aspects of the new theory of gravitation proposed in a recent paper are examined in greater detail. It is shown that in the smooth fluid approximation the familiar Einstein equations follow as a result of a specific conformal transformation. The equations of the the theory differ from those of Einstein in the neighbourhood of a particle, however. This is illustrated by means of an explicit solution. Criticisms of the theory by other authors are considered anid discussedt.
Cosmological models in a conformally invariant gravitational theory-I : The Friedmann model
(Wiley-Blackwell, 1972-01-27) Hoyle, F.; Narlikar, J. V.
The present paper discusses the formulation of the Friedmann cosmological models in terms of a conformally invariant ravitational theory. This theory is Machian in the sense that the mass of a particle arises from the interaction of the particle with a mass field m(X) generated by other particles. In cosmology the mass field m(X) at any particular space-time point X arises predominantly from particles at great distance from X. The Friedmann models are usually discussed in terms of the RobertsonWalker line element. It is known that this line element is conformal to the Minkowski line element ds² = dr²-d² -r² (d0 ² +sin² 0 dᵩ²). Cosmological space-time can therefore be transformed to Minkowski space-time by a suitable conformal transformation. It is not possible in the usual expositions to take advantage of this geometrical simplification because Einstein's gravitational equations are not conformally invariant. However, the present theory is conformally invariant so that transformation to Minkowski space is possible not only for the geometry but also for the physics. The three Friedmann cases k = 0, ± I are discussed in detail from this point of view. Although the cases k = ± I are spatially homogeneous in the Robertson-Walker frame they are not similarly homogeneous in the Minkowski frame, where they can be seen to represent only local clouds that happen to be symmetrically distributed with respect to an observer at r = o. This lack of homogeneity is not shared by the k = 0 case, which emerges from the analysis as the only model consistent with homogeneity in both frames, Robertson-Walker and Minkowski. The conformal transformation function between these two frames is singular at T = o. It is this mathematical breakdown of the transformation function which introduces the well-known singularity of the Friedmann models with respect to the Robertson-Walker frame--the singularity usually referred to as the origin of the Universe. From the present point of view this so-called origin does not arise physically at all. It turns out that the Universe possesses an opposite half, T < 0 in the Minkowski frame, which connects smoothly with ' our' half, T > o. Both halves of the Universe contribute to the mass function m(X), and are therefore connected physically. Indeed the appropriate form for m(X) appears to demand that both halves of the Universe be present. The half T < 0 is missed when the Robertson-Walker frame is used.
Cosmological models in a conformally invariant gravitational theory-II : A new model
(Wiley-Blackwell, 1972-01-27) Hoyle, F.; Narlikar, J. V.
Cosmology and action at a distance electrodynamics
(American Physical Society, 1995-04-24) Hoyle, F.; Narlikar, J. V.
This article reviews the developments in the electrodynamics of direct interparticle action, em-phasizing the achievements in quantum as well as classical electrodynamics. It is shown that the application of the Wheeler-Feynman absorber theory of radiation places stringent requirements on the asymptotic future and past light cones of the universe. All Friedmann cosmologies fail to meet these requirements, but the steady-state and the quasi-steady-state models have the right kind of structure to make the theory work. Further, it is shown that the working theory is free from the problems of divergence that trouble the classical and quantum field theory. In particular, no renormalization is needed: The bare mass and bare charge of an electron are finite. A few ideas relating to the response of the universe to a local microscopic experiment are presented as well as on possible clues to the outstanding issues of foundations of quantum theory
Cosmology and electrodynamics
(Nature Publishing Group, 1968-11-30) Hoyle, F.; Narlikar, J. V.
Cosmology and quantum electrodynamics
(Nature Publishing Group, 1968-07-27) Hoyle, F.; Narlikar, J. V.
Cosmology and quantum electrodynamics
(Nature Publishing Group, 1969-06-14) Hoyle, F.; Narlikar, J. V.
Direct particle theory of weak interactions
(-, 1972-01-01) Hoyle, F.; Narlikar, J. V.
A theory of weak interactions is developed in terms of direct particle action. In its simplest form the theory leads to the formulation given by Feynman and Gell-Mann.
Effect of quantum conditions in a Friedmann cosmology
(Nature Publishing Group, 1970-11-07) Hoyle, F.; Narlikar, J. V.
Electrodynamics of direct interparticle action I : The quantum mechanical response of the universe
(Academic Press, 1969-03-10) Hoyle, F.; Narlikar, J. V.
The present paper is the first of a series that seeks to obtain results in agreement with experience from a completely time-symmetric electromagnetic theory-i.e. which does not permit an ad hoc restriction to retarded solutions of time-symmetric equations. It is remarkable that the development of a wholly time-symmetric theory must be along lines entirely different from the usual electrodynamics. While a first quantisation of the particles can readily be carried out, there can be no separate quantisation of the field, since the field is wholly determined by the particles. This raises the question of how practical results that have hitherto been thought to arise from field quantisation can be obtained. The most immediate problem of this kind concerns the spontaneous transitions of atoms. Much of the present paper is directed toward showing that this problem can indeed be solved without the need for field quantisation. Although this question might appear simple compared to other issues in quantum e1ectrodynamics-e.g. vacuum polarisation-it is not trivial in its implication, for the establishment of one such case provides a critical precedent. The path integral method of first quantisation is used to demonstrate that provided the Universe is a perfect absorber along the future light cone the usual formulae for level shifts and for spontaneous transitions can be obtained in a steady-state model of the Universe, but not in open Friedmann models.
Electrodynamics of direct interparticle action II : Relativistic treatment of radiative processes
(Elsevier Science Publishers, 1971-01-21) Hoyle, F.; Narlikar, J. V.
Electromagnetic waves from very dense stars
(Nature Publishing Group, 1964-08-29) Hoyle, F.; Narlikar, J. V.; Wheeler, J. A.
Further astrophysical quantities expected in a quasi steady state universe
(EDP Sciences, 1994-02-06) Hoyle, F.; Burbidge, G.; Narlikar, J. V.
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 = 40 40⁹ years and P = 8 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 H₀¯¹. 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.
Light nuclei in the quasi-steady state cosmological model
(Springer, 1995-03-22) Hoyle, F.; Burbidge, G.; Narlikar, J. V.
Luminosity volume test and the local hypothesis of quasars
(Indian Academy of Sciences, 1986-01-28) Hoyle, F.; Narlikar, J. V.
It is shown that the luminosity-volume test for optically selected objects has an in-built bias towards increasing the average value of V/Vm above the Euclidean value of 1/2. A more satisfactory bias-free statistic is suggested in the form of In (V/Vm), The result of applying the test to a sample from the Bright Quasar Survey (BQS) shows that the local hypothesis of quasars is consistent with the data.
Mach's principle and the creation of matter
(Royal Society, 1962-11-27) Hoyle, F.; Narlikar, J. V.