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2 Pulsar Phenomenology

Many of the basic observational facts about radio pulsars were established shortly after their discovery [119Jump To The Next Citation Point] in 1967. Although there are still many open questions, the basic model has long been established beyond all reasonable doubt, i.e. pulsars are rapidly rotating, highly magnetised neutron stars formed during the supernova explosions of massive (>~~ 5-10 Mo .) stars. In the following, we discuss the observational properties that are most relevant to this review.


 2.1 The lighthouse model
 2.2 Pulse periods and slowdown rates
 2.3 Pulse profiles
 2.4 Interstellar dispersion and the pulsar distance scale
 2.5 Pulsars in binary systems
 2.6 Evolution of normal and millisecond pulsars
 2.7 Isolated recycled pulsars
 2.8 Pulsar velocities
 2.9 Current and future binary and millisecond pulsar search strategies
  2.9.1 All-sky searches
  2.9.2 Searches close to the plane of our Galaxy
  2.9.3 Searches at intermediate Galactic latitudes
  2.9.4 Targeted searches of globular clusters
  2.9.5 Current and future surveys
 2.10 Going further

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