Magnetohydrodynamic Acceleration of the Crab Pulsar Wind

Details Magnetohydrodynamic Acceleration of the Crab Pulsar Wind Magnetohydrodynamic Acceleration of the Crab Pulsar Wind

Jul 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...573l..31o&link_type=abstract

The Astrophysical Journal, Volume 573, Issue 1, pp. L31-L34.

Astronomy and Astrophysics

Astronomy

13

Ism: Magnetic Fields, Magnetohydrodynamics: Mhd, Stars: Pulsars: Individual: Name: Crab Pulsar, Stars: Winds, Outflows

Scientific paper

It is argued that ideal magnetohydrodynamic processes can realize the full acceleration of pulsar winds. The fast magnetosonic surface must be situated at the innermost points of the asymptotic domain far outside the Alfvénic distances. Ongoing field-flow interactions make plasma particles more and more ballistic, with the field structure becoming increasingly radial, in the asymptotic superfast domain. The condition of transfield force balance itself requires gradual conversion of Poynting flux to kinetic energy flux, thereby approaching a quasi-conical structure. This will be helpful to the resolution of the notorious discrepancy between the Crab pulsar wind theory and the Rees-Gunn model for the Crab Nebula.

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