Book contents
- Frontmatter
- Contents
- Preface
- Part I Discoveries and Techniques
- Part II Observed Physical Characteristics
- Part III Neutron Star Physics
- 13 Neutron Stars
- 14 Radius and Mass
- 15 Glitches, Timing Noise, Nudot Switching
- 16 Location and Geometry of Emitters
- 17 The Emission Mechanisms
- Part IV Environments and the Interstellar Medium
- References
- Index
17 - The Emission Mechanisms
from Part III - Neutron Star Physics
Published online by Cambridge University Press: 21 July 2022
Book contents
- Frontmatter
- Contents
- Preface
- Part I Discoveries and Techniques
- Part II Observed Physical Characteristics
- Part III Neutron Star Physics
- 13 Neutron Stars
- 14 Radius and Mass
- 15 Glitches, Timing Noise, Nudot Switching
- 16 Location and Geometry of Emitters
- 17 The Emission Mechanisms
- Part IV Environments and the Interstellar Medium
- References
- Index
Summary
Despite the extensive knowledge of the characteristics of the coherent radio emission, the mechanism is not understood. The high-energy radiation is incoherent and may be related to the flux of relativistic electrons and positrons in a current sheet at the boundary of the magnetosphere. The radio emission from the polar cap is at lower frequency at larger radii, as the magnetic field lines diverge. The emission may be affected by propagation through the polar cap; refraction along the magnetic field lines may increase the apparent pulse width at lower frequencies.
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- Information
- Pulsar Astronomy , pp. 280 - 296Publisher: Cambridge University PressPrint publication year: 2022