Pair formation and electric field boundary conditions at neutron star magnetic poles

Details Pair formation and electric field boundary conditions at neutron star magnetic poles Pair formation and electric field boundary conditions at neutron star magnetic poles

Sep 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980mnras.192..847j&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 192, Sept. 1980, p. 847-860.

Astronomy and Astrophysics

Astronomy

17

Boundary Conditions, Boundary Value Problems, Electric Fields, Magnetic Dipoles, Neutron Stars, Pair Production, Stellar Magnetic Fields, Angular Velocity, Earth Magnetosphere, Electron Acceleration, Photoionization, Positrons, Radio Emission, Stellar Rotation

Scientific paper

The paper gives the results of detailed calculations of pair formation in the inner magnetosphere of a neutron star made under the assumption that the surface electric field satisfies E . B = 0. It is assumed that high multipole components in the magnetic field increase the curvature of open flux lines and allow pair formation at the rotation period of the typical radio pulsar. Electron acceleration and pair formation have been considered previously by Arons & Scharlemann, but their electric field solution is shown here (in a one-dimensional approximation) to be unstable.
No dense pair plasma is formed, even in the absence of the instability. The outward moving plasma consists largely of a single stream of electrons so that for this boundary condition, there is no promising source of radio emission in the inner magnetosphere.
The conclusion is also valid for Ω . B < 0, where Ω is the neutron star angular velocity. The reverse flow of electrons from the photoelectric ionization of partially ionized 56Fe limits the parallel electric field component induced by ion inertia. Some consequences of the reverse flow of photoelectrons are discussed.

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