next up previous
Next: Finding Young Pulsars Up: Young Energetic pulsars Previous: Young Energetic pulsars

Basic Properties


tex2html_wrap_inline3922   t < 100,000 years
tex2html_wrap_inline3922   Short periods tex2html_wrap_inline4172 ms
tex2html_wrap_inline3922   Large period derivatives tex2html_wrap_inline4668
tex2html_wrap_inline3922   Strong magnetic fields tex2html_wrap_inline4672 Gauss
tex2html_wrap_inline3922   Close to Galactic plane

Table 1: Young Energetic Radio Pulsars. O - optical, X - X-rays, tex2html_wrap_inline2816 - tex2html_wrap_inline2816 -rays, I - infra-red, U - ultraviolet, J - jet, N - nebula, G - glicthes, BU - bullets, B - bow shock, Y - yes, P - probably, N - no, ? - maybe

tex2html_wrap_inline3922   Vast array of phenomena result from large


Figure 20: The radio pulsar equivalent of the Hertzsprung-Russell diagram - a physical diagram indicating the nature and evolution of neutron stars. Each dot represents a pulsar, stars represent pulsars associated with supernova remnants, circles indicate pulsars in binary systems and ellipses indicate pulsars in binary systems with eccentric orbits.

Jon Bell
Thu Dec 19 15:15:11 GMT 1996