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The stability of strong waves and its implications for pulsar wind shocks

MPG-Autoren
http://pubman.mpdl.mpg.de/cone/persons/resource/persons36454

Mochol,  Iwona
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

http://pubman.mpdl.mpg.de/cone/persons/resource/persons30680

Kirk,  John G.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

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Volltexte (frei zugänglich)

1310.5809.pdf
(Preprint), 249KB

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Zitation

Mochol, I., & Kirk, J. G. (2014). The stability of strong waves and its implications for pulsar wind shocks. Astronomische Nachrichten, 335(3), 256-261. Retrieved from http://arxiv.org/abs/1310.5809.


Zitierlink: http://hdl.handle.net/11858/00-001M-0000-0025-6827-C
Zusammenfassung
Strong waves can mediate a shock transition between a pulsar wind and its surroundings, playing the role of an extended precursor, in which the energy is effectively transferred from fields to non-thermal particles. The damping of such precursors results in an essentially unmagnetized shock near the equator. In this context, we discuss the stability of strong waves and its implications for the properties of shocks. Those with stable precursors can exist in the winds of most of isolated pulsars, but the precursors may be unstable if the external pressure in the nebula is high, as in Vela-like pulsars. Pulsar wind shocks in eccentric binary systems, such as B1259-63, can acquire precursors only at certain orbital phases, and this process should be accompanied by enhanced synchro-Compton and inverse Compton emission from the precursor. The same scenario may be at work in the binary HESS J0632+057.