The numerical simulation of nonstationary electron acceleration in a pulsar magnetosphere

Details The numerical simulation of nonstationary electron acceleration in a pulsar magnetosphere The numerical simulation of nonstationary electron acceleration in a pulsar magnetosphere

Dec 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987azh....64.1220r&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 64, Nov.-Dec. 1987, p. 1220-1232. In Russian.

Astronomy and Astrophysics

Astronomy

Electron Acceleration, Pulsar Magnetospheres, Pulsars, Stellar Atmospheres, Stellar Models, Brightness Temperature, Electron Bunching, Electron Energy, Radio Emission

Scientific paper

The energy of electrons accelerated stationarily inside the outflow channel is calculated in the framework of a globally self-consistent pulsar magnetosphere model. The stationary acceleration is shown to be almost always unstable. A numerical simulation of non-stationary electron acceleration is produced. It is shown that by the non-stationary acceleration the electron bunches are formed and the energy consumed by electrons inside the outflow channel increases by a few orders of magnitude as compared with that by the stationary acceleration. The energy consumed inside the outflow channel occurs to be sufficient for the pulsar radio emission energetics explanation, the radiopulsar phenomenon being explained as a thermal radio emission of the gas consisting of electron bunches. Such common properties of the pulsar radio emission as the high brightness temperature, the sharp radio emission directivity and the characteristic turn-over of the radio emission spectrum at the frequency of the order of 108Hz find a natural explanation in the framework of this model.

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