2019MNRAS.485..640J

Query : 2019MNRAS.485..640J

2019MNRAS.485..640J - Mon. Not. R. Astron. Soc., 485, 640-647 (2019/May-1)

The period-width relationship for radio pulsars revisited.

JOHNSTON S. and KARASTERGIOU A.

Abstract (from CDS):

In the standard picture of radio pulsars, the radio emission arises from a set of open magnetic field lines, the extent of which is primarily determined by the pulsar's spin period, P, and the emission height. We have used a data base of parameters from 600 pulsars to show that the observed profile width, W, follows W ∝ P–0.3 albeit with a large scatter, emission occurs from heights below 400 km and that the beam is underfilled. Furthermore, the prevalence in the data for long-period pulsars to have relatively wide profiles can only be explained if the angle between the magnetic and rotation axis decays with time.

Abstract Copyright: © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): pulsars: general

CDS comments: Misprints: PSR J1057-5552 and PSR J1057-5526 = PSR J1057-5226; PSR J1825-0925 = PSR J1825-0935.

Simbad objects: 10

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Number of rows : 10
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
2 PSR J1014-5719 Psr 10 15 37.96 -57 19 12.8           ~ 44 0
3 PSR J1028-5819 Psr 10 28 27.888 -58 19 06.14           ~ 122 1
4 PSR B1055-52 Psr 10 57 59.0450 -52 26 56.330           ~ 757 0
5 PSR J1141-6545 Psr 11 41 07.00060 -65 45 19.0500     25.08 24.38   ~ 207 1
6 PSR B1534+11 Psr 15 37 09.9603 +11 55 55.554           ~ 453 1
7 PSR B1607-52 Psr 16 11 03.20 -52 09 23.6           ~ 48 0
8 PSR B1822-09 Psr 18 25 30.62000 -09 35 22.0000           ~ 382 0
9 PSR J1906+0749 Psr 19 06 48.67 +07 46 28.6           ~ 172 1
10 PSR J1915+1606 Psr 19 15 27.99999 +16 06 27.4034     22.5     ~ 1032 1

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