The properties of fully relativistic rotating hadron star models are discussed using models based on recently developed equations of state. All of these stable neutron star models are bound with binding energies as high as ∼ 25%. During hadron star formation, much of this energy will be released. The consequences, resulting from the release of this energy, are examined.

The problem of the development of the angular velocity distribution during the final phase of gravitational contraction of a star immediately prior to the onset of degeneracy and during the subsequent cooling phase is surveyed. Processes that may affect this distribution are discussed at some length, and estimates of the timescales for redistribution of the angular momentum are given for each process. Possible effects on the evolution and observable consequences are briefly considered.

We discuss some of the effects which magnetic fields in the range 104–108 G have on the continuum emission of white dwarfs. In order to show how atomic processes are related to the transport of radiation in an anisotropic medium we introduce the radiative transfer equation for polarized light. Using this transfer equation as a guide we develop a greatly simplified model of a white dwarf atmosphere: anisotropic absorption of unpolarized light passing through a cold, optically-thin layer. Two possible sources of continuum polarization in white dwarfs with strong magnetic fields are explored, namely bound-free transitions and cyclotron absorption. Within the hydrogenic approximation we develop a further approximation which is valid for bound-free transitions when B is in the range 104–107 G. Using this approximation it is possible to obtain simple expressions for the net circular and linear polarization in terms of the zero-field opacity. In the case of cyclotron absorption, the cross section is large and strongly peaked at the cyclotron frequency, which falls in the infrared or optical for B ⩾ 108 G. This process can lead to net circular and linear polarization of comparable magnitude. For stars with non-uniform magnetic fields, the cyclotron absorption effects are spread over considerable wavelength ranges, with possibly quite complicated wavelength-dependent polarization.

We present the recent results of our continuing program of investigation of the behavior of matter in strong to super-strong magnetic fields (B ∼ 106−1012 G). This work was motivated by the discovery of strong magnetic fields (B ∼ 107 G) in some white dwarfs and the likely existence of super-strong fields (B ∼ 1012 G) in pulsars. Magnetic white dwarfs were discovered from observations of the continuous spectrum and one of the most intriguing challenges for the theorist is to provide an explanation for the observed wavelength dependence of the fractional circularly and linearly polarized radiation. Our initial response to this question was the determination of an exact solution of Kemp's harmonic oscillator model. These results are used as input to the ATLAS model atmosphere program and then comparison is made with observations. The disparities still existing between theory and observation convince us of the necessity for developing a new model of the continuum radiation, two likely possibilities being photoionization and free-free absorption. This leads us to present a general formulation of radiation absorption and emission processes in a magnetic field. Next we calculate the cross section for the photoionization, correct to first order in B. For the purpose of obtaining exact results for this cross section, the effect of a magnetic field on the energy spectrum and wave functions of hydrogen, helium, etc. must be obtained. The results for hydrogen are presented here. They will be useful also in determining accurate values for the displacements due to the quadratic Zeeman effect in the line spectra of DA stars, particularly for the higher excited states.

I shall report on some work done in France in the last few years concerning the possible existence of antimatter in the Universe. It will be shown that, by taking due account of several physical effects which have been theoretically predicted, one can propose a coherent theory for the origin of matter and galaxies that appears to be quantitatively satisfactory. In this model there should exist as many antigalaxies as galaxies. During the course of this paper, I shall try to make it clear what the basic physical processes are and the present state of their investigation. This discussion will therefore be restricted to the two aforementioned problems, viz., the origin of matter and protogalaxies, leaving aside other astrophysical applications.

The lagging core model for quasars (i.e., ‘white holes’) is shown to impose a negative exponential for the number of quasars at any given time as measured from the start of the cosmological expansion. Models in which quasars and other dense cores result from collapse yield a different behavior. A recent observational count appears to fit a negative exponential.