On the structure of the inner Crab Nebula

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Abstract

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.

Original languageEnglish
Pages (from-to)L34-L36
JournalMonthly Notices of the Royal Astronomical Society
Volume329
Issue number2
DOIs
StatePublished - 11 Jan 2002

Keywords

  • ISM: individual: crab nebula
  • ISM: jets and outflows
  • MHD
  • Shock waves pulsars: general
  • Supernova remnants

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