No pulsar left behind - I. Timing, pulse-sequence polarimetry and emission morphology for 12 pulsars

被引：16

作者：

Brinkman, Casey ^{[1
]}

Freire, Paulo C. C. ^{[2
]}

Rankin, Joanna ^{[1
,3
]}

Stovall, Kevin ^{[4
]}

机构：

[1] Univ Vermont, Dept Phys, Burlington, VT 05401 USA

[2] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany

[3] Univ Amsterdam, Anton Pannekoek Inst Astron, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

[4] Natl Radio Astron Observ, POB 0, Socorro, NM 87801 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2018年 / 474卷 / 02期

基金：

美国国家科学基金会; 美国国家航空航天局;

关键词：

polarization; astrometry; pulsars: general; pulsars: individual: PSR J0627+0706; pulsars: individual: PSR J2053+1718; CENTRAL COMPACT OBJECTS; GAMMA-RAY PULSARS; MILLISECOND PULSARS; SUPERNOVA REMNANT; RECYCLED PULSARS; EMPIRICAL-THEORY; X-RAY; GEOMETRY; REGION;

D O I：

10.1093/mnras/stx2842

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

In this paper, we study a set of 12 pulsars that previously had not been characterized. Our timing shows that eleven of them are 'normal' isolated pulsars, with rotation periods between 0.22 and 2.65 s, characteristic ages between 0.25 Myr and 0.63 Gyr, and estimated magnetic fields ranging from 0.05 to 3.8 x 10(12) G. The youngest pulsar in our sample, PSR J0627+0706, is located near the Monoceros supernova remnant (SNR G205.5+0.5), but it is not the pulsar most likely to be associated with it. We also confirmed the existence of a candidate from an early Arecibo survey, PSR J2053+1718, its subsequent timing and polarimetry are also presented here. It is an isolated pulsar with a spin period of 119 ms, a relatively small magnetic field of 5.8 x 10(9) G and a characteristic age of 6.7Gyr; this suggests the pulsar was mildly recycled by accretion from a companion star, which became unbound when that companion became a supernova. We report the results of single-pulse and average Arecibo polarimetry at both 327 and 1400 MHz aimed at understanding the basic emission properties and beaming geometry of these pulsars. Three of them (PSRs J0943+2253, J1935+1159 and J2050+1259) have strong nulls and sporadic radio emission, several others exhibit interpulses (PSRs J0627+0706 and J0927+2345) and one shows regular drifting subpulses (J1404+1159).

引用

页码：2012 / 2027

页数：16

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