It is known from observations that pulsars are high velocity objects. As a sizable fraction of these collapsars originates from low velocity single stars, they must have received a “kick” velocity at their birth. Which we assume to be due to the asymmetry of the SN-explosion and to be randomly orientated. Hanson (1979) estimated this asymmetric velocity in a statistical study to be about 102 km s−1. For SNe occurring in binaries the runaway velocities depend on the initial conditions. According to hydrodynamical calculations by Fryxell and Arnett (1979) the momentum imparted by the SN shell to the companion is some 80% of the momentum incident on the geometric cross-section of the star. This is due to mass stripping, which reduces the radius of stars with extended atmospheres, and to a smooth flow of the SN shell around the spherical companion and the nearly spherically symmetric ablation of some mixed stellar material. The mass loss of the companion is negligible.

Recent developments in the theory of the light from supernovae indicate that while Type II supernovae probably involve the explosion of a massive star with an extended envelope, Type I supernovae may involve the total thermonuclear disruption of a white dwarf. The energy release in a Type II supernova is presumably related to the contraction of the core to a neutron star and pulsar formation is likely. The hypothesis that Type II supernovae leave pulsars while Type I supernovae do not leave compact remnants is shown to be consistent with the available information on X-ray sources containing neutron stars, young supernova remnants, and the distribution of pulsars in the galaxy. Some pulsars are probably formed in the explosion of a massive star that has lost its envelope. These events may not be accompanied by a bright supernova display.

We use the recently introduced concept of a “window” of magnetic field strengths in which pulsars can be active to explain the variation in morphology of supernova remnants. Neutron stars created with field strengths of a value permitting pulsar activity result in particle production and Crab-like centrally concentrated remnants. Other field values lead to strong magnetic dipole radiation and consequent shell formation, e.g., Cas A.

The galactic distribution of pulsars follows the general form of many population I objects in galactocentric radius, but has a wide distribution above and below the galactic plane due to high space velocities imparted to the pulsars at birth. The evidence for this model is described and the various factors involved in estimating the total galactic population and the galactic birthrate of pulsars are discussed. The various estimates of the galactic population which cluster around 5 × 105 are seen to be critically dependent upon the cut-off at low luminosities and upon the value of the mean electron density within 500 pc of the Earth. Estimates of the lifetimes of pulsars are available from both the characteristic ages and proper motion measurements and both give values of about 5 million years. The implied birthrate of one in every 10 years is barely compatible with most estimates of the galactic supernova rate.

At the end of 1978 the results of the second pulsar survey at the Molonglo Observatory (Manchester et al., 1978) and of a new survey of the northern hemisphere made at Green Bank (Damashek et al., 1978) were published. More than 80% of the celestial sphere were thus searched for pulsars in a careful and homogeneous manner. As a result of these surveys 172 new pulsars were discovered and parameters of 95 previously known pulsars were improved. Recently two new pulsars were discovered in the Pushino Observatory (Alekseyev et al., 1979), bringing the grand total of known pulsars to 325.

The distribution of pulsars in galactocentric radius and z distance has been determined for opposite halves of the Galaxy, using data on 328 pulsars from three surveys. The distributions in galactocentric radius are found to be significantly different at positive and negative longitudes, although both show strong peaks between 5 and 6 kpc. There is also some indication that pulsars are located preferentially along spiral arms. Distributions in the z component of dispersion measure above and below the galactic plane also show asymmetry, with higher dispersion occurring at negative z. This may imply the existence of a narrow (~ 100 pc), high electron density layer below the plane of the Sun in the inner galaxy.

The second Molongo pulsar survey (Manchester et al., 1978) provides a large sample of pulsars in the southern sky. It is of interest to obtain non-dispersion-dependent distances for as many of these pulsars as possible. Since most of these pulsars are relatively weak, a system of high sensitivity is required. In this paper we report on preliminary observations made at Parkes during June 1980 with such a system.

I am afraid the best I can do on the next few pages is to convey the personal impressions that I have been left with after listening to sixty odd talks on almost every topic connected with pulsars. It is obviously impossible even to mention, leave alone comment on, each one of the papers that have been presented in these four packed days. Those few I touch upon will naturally reflect my personal biases for which I ask that you please bear with me.