Pulsar emission

Abstract

A considerable improvement is made in an equation for a pulsar’s radio luminosity that we derived earlier. From the observed radio luminosity L₀, the new equation enables one to calculate the magnetic moment m of the pulsar’s neutron star:$\mu \approx 5.13 \cdot 10^{15} P^{{\raise0.5ex\hbox{$\scriptstyle 4$}\kern-0.1em/\kern-0.15em\lower0.25ex\hbox{$\scriptstyle 7$}}} \sqrt {L_0 }$, whereP s the pulsar’s period. Equations are derived for the fluxes of pulsar energy due to g-ray emission and ultrarelativistic electrons escaping from the pulsar’s channels of open magnetic field lines. Assuming that the lengthening of pulsar periods is due to these channels of loss of rotational energy, an equation is derived for the moment of inertia of the neutron star:$I \approx 1.15 \cdot 10^{23} (1 + 5.35 \cdot 10^{ - 4} P^{{\raise0.5ex\hbox{$\scriptstyle {19}$}\kern-0.1em/\kern-0.15em\lower0.25ex\hbox{$\scriptstyle {21}$}}} L_0^{{\raise0.5ex\hbox{$\scriptstyle 1$}\kern-0.1em/\kern-0.15em\lower0.25ex\hbox{$\scriptstyle 8$}}} )P^{15/7} L_0^{1/3} /\dot P$, where is the rate of increase in the period and L₀ is the radio luminosity.