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The magnetic fields of neutron stars


tex2html_wrap_inline3922   tex2html_wrap_inline4056
tex2html_wrap_inline3922   Typically tex2html_wrap_inline4060 Gauss for normal pulsars
tex2html_wrap_inline3922   Consistent with flux conservation during stellar collapse
tex2html_wrap_inline3922   Typically tex2html_wrap_inline4066 Gauss for millisecond pulsars
tex2html_wrap_inline3922   Gravity dominates stellar structure
tex2html_wrap_inline3922   B field dominates exterior


tex2html_wrap_inline3922   Stellar surface is so small that observed emission is dominated by the magnetic field.
tex2html_wrap_inline3922   The electromagnetic wave generated by the misaligned rotating dipole causes loss of rotational energy and accounts for the observed slowdown
tex2html_wrap_inline3922   Only field lines inside light cylinder are closed
tex2html_wrap_inline3922   Particles are constrained move along field lines

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