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.
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页数：12
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