On the nature of radio pulsars with long periods

被引：12

作者：

Lomiashvili, D

Machabeli, G

Malov, I

机构：

[1] Tbilisi State Univ, GE-0128 Tbilisi, Georgia

[2] Abastumani Astrophys Observ, Tbilisi, Georgia

[3] PN Lebedev Phys Inst, Pushchino Radio Astron Observ, Pushchino 142290, Russia

[4] Isaac Newton Inst Chile, Pushchino, Moscow Region, Russia

来源：

ASTROPHYSICAL JOURNAL | 2006年 / 637卷 / 02期

关键词：

pulsars : individual (PSR J1119-6127; PSR J1814-1744; PSR J1847-0130; PSR J2144-3933); stars : magnetic fields;

D O I：

10.1086/498419

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We show that the drift waves near the light cylinder can cause modulation of the emission with periods of the order of several seconds. These periods explain the intervals between successive pulses observed in `` magnetars'' and radio pulsars with long periods. The model under consideration makes it possible to calculate the real rotation periods of the host neutron stars. They are less than 1 s for the investigated objects. The magnetic fields at the surface of the neutron star are of the order of 10(11) - 10(13) G and equal to the usual fields for known radio pulsars.

引用

页码：1010 / 1015

页数：6

共 27 条

[1] PAIR CREATION ABOVE PULSAR POLAR CAPS - STEADY FLOW IN THE SURFACE ACCELERATION ZONE AND POLAR-CAP X-RAY-EMISSION [J].