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The σ Problem of the Crab Pulsar Wind

Published online by Cambridge University Press:  19 July 2016

J. G. Kirk  and
O. Skjæraasen
J. G. Kirk
Affiliation:
Max-Planck-Institut für Kernphysik, Postfach 10 39 80, 69029 Heidelberg, Germany
O. Skjæraasen
Affiliation:
Observatoire de Strasbourg, 11 rue de l'Université, F-67000 Strasbourg, France

Abstract

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The conversion of the Crab pulsar wind from one dominated by Poynting flux close to the star to one dominated by particle-borne energy at the termination shock is considered. The idea put forth by Coroniti (1990) and criticized by Lyubarsky & Kirk (2001) that reconnection in a striped wind is responsible, is generalized to include faster prescriptions for the a priori unknown dissipation rate. Strong acceleration of the wind is confirmed, and the higher dissipation rates imply complete conversion of Poynting flux into particle-borne flux within the unshocked wind.

Type
Part 4: Pulsar Wind Nebulae and Their Environments
Information
Symposium - International Astronomical Union , Volume 218: Young Neutrons Stars and their Environments , 2004 , pp. 171 - 174
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Arons, J. 1979, Space Sci. Rev., 24, 437.CrossRefGoogle Scholar
Beskin, V. S., Kuznetsova, I. V., & Rafikov, R. R. 1998, MNRAS, 299, 341.CrossRefGoogle Scholar
Bogovalov, S., & Tsinganos, K. 1999, MNRAS, 305, 211.CrossRefGoogle Scholar
Buckley, R. 1977, MNRAS, 180, 125.CrossRefGoogle Scholar
Chiueh, T., Li, Z.-Y., & Begelman, M. C. 1998, ApJ, 505, 835.CrossRefGoogle Scholar
Contopoulos, I., & Kazanas, D. 2002, ApJ, 566, 336.CrossRefGoogle Scholar
Coroniti, F. V. 1990, ApJ, 349, 538.CrossRefGoogle Scholar
Emmering, R. T., & Chevalier, R. A. 1987, ApJ, 321, 334.CrossRefGoogle Scholar
Gallant, Y. A., van der Swaluw, E., Kirk, J. G., & Achterberg, A. 2002, in ASP Conf. Ser., Vol. 271, Neutron Stars in Supernova Remnants, eds. Slane, P. O., & Gaensler, B. M., (San Francisco: ASP), p. 99.Google Scholar
Harris, E. G. 1962, Nuovo Cimento, 23, 115.CrossRefGoogle Scholar
Hibschman, J. A., & Arons, J. 2001, ApJ 560, 871.CrossRefGoogle Scholar
Hoh, F. C. 1968, Physics Fluids, 9, 277.CrossRefGoogle Scholar
Kennel, C. F., & Coroniti, F. V. 1984, ApJ, 283, 694.CrossRefGoogle Scholar
Kirk, J. G., & Skjæraasen, O. 2003, ApJ, 591, 366.CrossRefGoogle Scholar
Kirk, J. G., Skjæraasen, O., & Gallant, Y. A. 2002, A&A, 388, L29.Google Scholar
Lyubarsky, Y. 1996, A&A, 311, 172.Google Scholar
Lyubarsky, Y. 2002, MNRAS, 329, L34.CrossRefGoogle Scholar
Lyubarsky, Y., & Eichler, D. 2001, ApJ, 562, 494.CrossRefGoogle Scholar
Lyubarsky, Y., & Kirk, J. G. 2001, ApJ, 547, 437.CrossRefGoogle Scholar
Rees, M. J., & Gunn, J. E. 1974, MNRAS, 167, 1.CrossRefGoogle Scholar