Radio Pulsars

被引:19
作者
Beskin, V. S. [1 ,2 ]
Chernov, S. V. [3 ]
Gwinn, C. R. [4 ]
Tchekhovskoy, A. A. [5 ]
机构
[1] Russian Acad Sci, Lebedev Phys Inst, Moscow 119991, Russia
[2] Moscow Inst Phys & Technol, Dolgoprudnyi 141700, Moscow Region, Russia
[3] Russian Acad Sci, Lebedev Phys Inst, Moscow 117997, Russia
[4] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA
[5] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA
基金
俄罗斯基础研究基金会; 美国国家科学基金会;
关键词
Neutron stars; Pulsars; ACCRETION-INDUCED COLLAPSE; FORCE-FREE MAGNETOSPHERE; ROTATING NEUTRON-STARS; MILLISECOND PULSAR; EMPIRICAL-THEORY; EMISSION REGION; POPULATION SYNTHESIS; WAVE-PROPAGATION; CRAB-NEBULA; POLAR CAPS;
D O I
10.1007/s11214-015-0173-8
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Almost 50 years after radio pulsars were discovered in 1967, our understanding of these objects remains incomplete. On the one hand, within a few years it became clear that neutron star rotation gives rise to the extremely stable sequence of radio pulses, that the kinetic energy of rotation provides the reservoir of energy, and that electromagnetic fields are the braking mechanism. On the other hand, no consensus regarding the mechanism of coherent radio emission or the conversion of electromagnetic energy to particle energy yet exists. In this review, we report on three aspects of pulsar structure that have seen recent progress: the self-consistent theory of the magnetosphere of an oblique magnetic rotator; the location, geometry, and optics of radio emission; and evolution of the angle between spin and magnetic axes. These allow us to take the next step in understanding the physical nature of the pulsar activity.
引用
收藏
页码:207 / 237
页数:31
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