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Pulsar distances are obtained from their frequency dispersion, geometrically from annual parallax, and from optical identifiction with supernova remnants, globular clusters and binary companions. For most pulsars, distances are only available from observation of effects of propagation in the interstellar medium, particularly neutral hydrogen absorption and frequency dispersion. Interpretation of the dispersion measure requires a model of the electron distribution through the Galaxy.
Many of the masses of pulsars in binary systems are known to high accuracy from their dynamics, while the masses of solitary pulsars are difficult to obtain. Radii are available from x-ray luminosity where this is known to be thermal. This chapter assembles the known measurements of mass and radius for all neutron stars.
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