Hostname: page-component-cd9895bd7-jn8rn Total loading time: 0 Render date: 2024-12-26T03:17:59.586Z Has data issue: false hasContentIssue false
  • English
  • Français

The Termination Shock in a Striped Pulsar Wind

Published online by Cambridge University Press:  19 July 2016

Yury Lyubarsky
Yury Lyubarsky*
Affiliation:
Ben-Gurion University, P.O.B. 653, Beer-Sheva 84105, Israel

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.

Toroidal stripes of opposite magnetic polarity are formed in the equatorial belt of the wind emanating from an obliquely rotating pulsar magnetosphere. Such a striped wind transfers most of its spindown energy because the angular distribution of the energy flux in the pulsar wind is maximum at the equator. The alternating field annihilates either in the pulsar wind or at the termination shock so that the flow in the equatorial belt downstream of the termination shock is weakly magnetized. At high latitudes, the magnetization of the flow is higher than in the equatorial belt whereas the total energy flux is smaller. At such a distribution of the energy flux and magnetization, the downstream flow separates into an equatorial disk and a magnetically collimated polar jet. Particle acceleration at the termination shock in a striped wind is discussed. It is argued that the radio emitting electrons are accelerated by driven reconnection of the alternating field at the shock whereas the Fermi acceleration of electrons preaccelerated in the reconnection process results in a high energy tail responsible for the X- and γ-ray emission.

Type
Part 4: Pulsar Wind Nebulae and Their Environments
Information
Symposium - International Astronomical Union , Volume 218: Young Neutrons Stars and their Environments , 2004 , pp. 167 - 170
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Bietenholtz, M. F., Frail, D. A., & Hester, J. J. 2001, ApJ, 560, 254.Google Scholar
Bogovalov, S. V. 1999, A&A, 349, 101.Google Scholar
Bogovalov, S. V., & Khangoulian, D. V. 2002, MNRAS, 336, L53.CrossRefGoogle Scholar
Chiueh, T., Li, Z.-Y., & Begelman, M. C. 1998, ApJ, 505, 835.CrossRefGoogle Scholar
Gallant, Y. A. 2002, in Relativistic Flows in Astrophysics (Lecture Notes in Physics Vol. 589), eds. Guthmann, A.W. et al., (New York: Springer), p. 24.Google Scholar
Gallant, Y. A., & Tuffs, R. J. 2002, in ASP Conf. Series, Vol. 271, Neutron Stars in Supernova Remnants, eds. Slane, P. O., & Gaensler, B. M., (San Francisco: ASP), p. 161.Google Scholar
Hester, J. J. et al. 2002, ApJ, 577, L49.Google Scholar
Kennel, C. F., & Coroniti, F. V. 1984, ApJ, 283, 694.Google Scholar
Kirk, J. G., & Skjæraasen, O. 2003, ApJ, 591, 366.Google Scholar
Komissarov, S. S., & Lyubarsky, Y. E. 2003, MNRAS, 344, L93.Google Scholar
Komissarov, S. S., & Lyubarsky, Y. E. 2004, MNRAS, 349, 779.Google Scholar
Lyubarsky, Y. E. 2002, MNRAS, 329, L34.Google Scholar
Lyubarsky, Y. E. 2003a, MNRAS, 339, 765.Google Scholar
Lyubarsky, Y. E. 2003b, MNRAS, 345, 153.Google Scholar
Lyubarsky, Y. E., & Eichler, D. 2001, ApJ, 562, 494.Google Scholar
Lyubarsky, Y. E., & Kirk, J. G. 2001, ApJ, 547, 437.Google Scholar
Pavlov, G. G., Teter, M. A., Kargaltsev, O. Y., & Sanwal, D. 2003, ApJ, 591, 1157.Google Scholar
Rees, M. J., & Gunn, J. E. 1974, MNRAS, 167, 1.Google Scholar
Shklovsky, I. S. 1970, ApJ, 159, L77.Google Scholar