Luminosities of radio Pulsars

Abstract

Luminosity is an intrinsic property of radio pulsars related to the properties of the magnetospheric plasma and the beam geometry, and inversely proportional to the observing frequency. In traditional models, luminosity has been considered as a function of the spin parameters of pulsars. On the other hand, parameter independent models like power law and lognormal have been also used to fit the observed luminosities. Some of the older studies on pulsar luminosities neglected observational biases, but all of the recent studies tried to model observational effects as accurately as possible. Luminosities of pulsars in globular clusters and in the Galactic disk have been studied separately. Older studies concluded that these two categories of pulsars have different luminosity distributions, but the most recent study concluded that those are the same. This article reviews all significant works on pulsar luminosities and discusses open questions.

Invited review in International Journal of Modern Physics D. 21 pages, 8 tables, 3 figures

References in corpus (7)

• The ATNF Pulsar Catalogue
• The pulsar spectral index distribution
• Stellar Encounter Rate in Galactic Globular Clusters
• Population synthesis of radio and gamma-ray millisecond pulsars from the Galactic disk
• A 1.4-GHz Arecibo Survey for Pulsars in Globular Clusters
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• TRAPUM search for pulsars in supernova remnants and pulsar wind nebulae -- I. Survey description and initial discoveries
• A stacked search for spatial coincidences between IceCube neutrinos and radio pulsars
• Search for Dyson rings around pulsars: unexpected light curves
• Distances of Galactic Radio Pulsars; First Quadrant: $-2^{\circ }<\ell <90^{\circ }$ and $-2^{\circ }<b<2^{\circ }$
• Investigating four new candidate redback pulsars discovered in the image plane
• Application of Efron-Petrosian method to radio pulsar fluxes
• Neutron stars in the light of SKA: Data, statistics, and science