Estimates of the Surface Magnetic Field Strength of Radio Pulsars

被引：1

作者：

Kim, Vitaliy ^{[1
,2
]}

Umirbayeva, Adel ^{[1
,3
]}

Aimuratov, Yerlan ^{[1
,3
,4
]}

机构：

[1] Fesenkov Astrophys Inst, Observ 23, Alma Ata 050020, Kazakhstan

[2] Pulkovo Observ, Pulkovoskoe Shosse 65-1, St Petersburg 196140, Russia

[3] Al Farabi Kazakh Natl Univ, Fac Phys & Technol, Dept Theoret & Nucl Phys, Al Farabi Ave 71, Alma Ata 050040, Kazakhstan

[4] Int Ctr Relativist Astrophys Network, Piazza Repubbl 10, I-65122 Pescara, Italy

来源：

UNIVERSE | 2023年 / 9卷 / 07期

关键词：

neutron star; radio pulsar; magnetic dipole radiation; magnetic field; EVOLUTION; ANGLE;

D O I：

10.3390/universe9070334

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We investigate the geometry of the magnetic field of rotation-powered pulsars. A new method for calculating an angle (beta) between the spin and magnetic dipole axes of a neutron star (NS) in the ejector stage is considered within the frame of the magnetic dipole energy loss mechanism. We estimate the surface magnetic field strength (B-ns) for a population of known neutron stars in the radio pulsar (ejector) stage. The evaluated B-ns(beta) may differ by an order of magnitude from the values without considering the angle beta. It is shown that B-ns(beta) lies in the range 10(8)-10(14) G for a known population of short and middle periodic radio pulsars.

引用

页数：12

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