The radio luminosity of pulsars

Details The radio luminosity of pulsars The radio luminosity of pulsars

Jan 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...171..152s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 171, no. 1-2, Jan. 1987, p. 152-156.

Astronomy and Astrophysics

Astrophysics

37

Pulsars, Radio Spectra, Stellar Luminosity, Pulsar Magnetospheres, Stellar Magnetic Fields

Scientific paper

A suggestion is offered that may solve an inconsistency regarding the luminosity/period relationships of pulsars. Although the relation seems to be consistent with the observed luminosities, Stollman (1986) showed that it predicts far too many pulsars with both low field strengths and short periods. It is shown that the observed radio luminosities, L, of pulsars can be described in terms of the parameter B/P-squared. If the assumption is made that the luminosity is proportional to the potential drop across the polar gap in the magnetosphere of the pulsar, then this dependence of L on B/P-squared can be understood within a simple physical picture. Further support for this luminosity law comes from the fact that it generates a distribution of pulsars in the B vs. P diagram that is similar to the observed one.

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