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
13 - Neutron Stars
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
Stable neutron stars exist with masses approximately between one and two solar masses, and radii of approximately 10 to 11 km. The structure is determined primarily by a balance between gravitation and the repulsion between adjacent neutrons. The configuration depends on the equation of state of the neutron fluid. The rotation of the strong dipolar magnetic field generates a magnetosphere of charged particles, which co-rotates with the star.
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- Pulsar Astronomy , pp. 213 - 225Publisher: Cambridge University PressPrint publication year: 2022