Observations of the mean profiles of radio pulsars and the structures of their emitting regions at 102 MHz

Details Observations of the mean profiles of radio pulsars and the structures of their emitting regions at 102 MHz Observations of the mean profiles of radio pulsars and the structures of their emitting regions at 102 MHz

May 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999arep...43..288k&link_type=abstract

Astronomy Reports, Volume 43, Issue 5, May 1999, pp.288-304

Astronomy and Astrophysics

Astronomy

15

Scientific paper

The mean profiles of 104 pulsars at 102 MHz are presented. The sample includes 45 pulsars not previously observed at frequencies lower than 400 MHz, including 21 ms and short-period pulsars (P <= 50 ms). A compensation for profile broadening due to the interstellar medium is performed for pulsars with large dispersion measures and for short-period pulsars. Component analyses describing the mean profiles as superpositions of Gaussian components are given. The number of components detected depends on the signal-to-noise ratio (SNR). A SNR of at least 50 is required for an informative analysis of the profile structure. At lower SNR, weak features may be "swamped" by the noise, and the structure that is determined may be incomplete. In general, the mean profiles show a more complex multicomponent structure than previously believed; for a number of pulsars, six and even seven components were detected. This type of structure cannot be explained by the standard model for the emitting region, consisting of inner and outer hollow cones and a central source. The observations support the hypothesis that the emitting region has the form of a beam of radiating particles injected from discrete regions of discharge near the polar caps. The dependence of the profile width on the period is analyzed, and the height of the emitting region is estimated. For 102 MHz, r_102 ~= (0.8-2.3) x 10^7 cm ~= (2-5) x 10^-3r_LC for a period of P = 1 s, and r_102 ~= (2-5) x 10^6 cm ~= (0.04-0.1)r_LC for a period of P = 10 ms, where r_LC is the radius of the light cylinder. The scattering widths are measured for 43 of the pulsars. The dispersion-measure dependence tau_sc(DM) propto DM^(2-2.5) is close to the relation expected from theory.

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