Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999ap.....42..190s&link_type=abstract
Astrophysics, Volume 42, Issue 2, pp.190-200
Astronomy and Astrophysics
Astrophysics
Scientific paper
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:μ ≈ 5.13 \cdot 10^{15} P^{{raise0.5exhboxriptstyle 4kern-0.1em/kern-0.15emlower0.25exhboxriptstyle 7}} sqrt {L_0 } , where P 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 ≈ 1.15 \cdot 10^{23} (1 + 5.35 \cdot 10^{ - 4} P^{{raise0.5exhboxriptstyle {19}kern-0.1em/kern-0.15emlower0.25exhboxriptstyle {21}}} L_0^{{raise0.5exhboxriptstyle 1kern-0.1em/kern-0.15emlower0.25exhboxriptstyle 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.
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