Hostname: page-component-cd9895bd7-jkksz Total loading time: 0 Render date: 2024-12-23T18:45:46.807Z Has data issue: false hasContentIssue false
  • English
  • Français

Pulsar Spin-Down by 3P2 Superfluid Neutrons

Published online by Cambridge University Press:  26 May 2016

Xin-Lian Luo ,
Qiu-He Peng ,
Ming Zhang  and
Chih-Kang Chou
Xin-Lian Luo
Affiliation:
Department of Astronomy, Nanjing University, Nanjing 210093, China
Qiu-He Peng
Affiliation:
Department of Astronomy, Nanjing University, Nanjing 210093, China
Ming Zhang
Affiliation:
Department of Astronomy, Nanjing University, Nanjing 210093, China
Chih-Kang Chou
Affiliation:
Institute of Astronomy and Department of Physics, National Central University, Chung-Li Taiwan 32054, China Taipei

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

To describe pulsar spin-down, a simple combined torque model, that takes into account both the standard magnetic dipole radiation and the electromagnetic radiation from the 3P2 superfluid vortex neutrons inside neutron star, is presented. Using an ordinary exponential model for the magnetic field decay, we investigate pulsar evolution tracks on the diagram, which is quite different from that of the standard magnetic dipole radiation model, especially when the superfluid torque or field decay become dominate.

Type
Part 5 Pulsars and Other Neutron Stars
Information
Symposium - International Astronomical Union , Volume 214: High Energy Processes and Phenomena in Astrophysics , 2003 , pp. 175 - 176
Copyright
Copyright © Astronomical Society of the Pacific 2003 

References

Huang, J. H. et al. 1982, A&A, 113, 9 Google Scholar
Luo, X. L., Peng, Q. H. and Chou, C. K. 2002, Chin. Phys. Lett, Submitted Peng, Q. H. et al. 1982, A&A, 107, 258 Google Scholar