On the structure of the inner Crab Nebula

Details On the structure of the inner Crab Nebula On the structure of the inner Crab Nebula

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mnras.329l..34l&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 329, Issue 2, pp. L34-L36.

Astronomy and Astrophysics

Astronomy

37

Mhd, Shock Waves, Pulsars: General, Ism: Individual: Crab Nebula, Ism: Jets And Outflows, Supernova Remnants

Scientific paper

Origin of the jet-like feature in the inner Crab Nebula is discussed. Because self-collimation processes in ultrarelativistic pulsar winds are extremely ineffective, it is suggested that the collimation occurs beyond the termination shock where the flow is already mildly (or non-) relativistic. It is argued that the shock shape is highly non-spherical because the energy flux in the pulsar wind decreases towards the axis. The shock near the axis should be much closer to the pulsar than at the equator and therefore the jet looks as if it originates directly from the pulsar.

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