Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995azh....72..826i&link_type=abstract
Astronomicheskij Zhurnal, vol. 72, p. 826
Astronomy and Astrophysics
Astronomy
3
Neutron Stars, Stellar Magnetospheres, Gamma Ray Bursts, Astronomical Models, Electron-Positron Plasmas, Polar Regions, Radio Emission, Stellar Rotation, Electron-Positron Pairs, Electric Fields
Scientific paper
If the rotational period for a magnetized neutron star exceeds a certain limit, it cannot be a pulsar. In this case, electron-positron plasma does not form in the polar regions of the magnetosphere on open field lines, where its flow generates the observed radio emission. This does not mean, however, that e(+)e(-) pairs do not form in closed regions of the magnetosphere in more slowly rotating neutron stars. The potential difference between the equator and the poles is 10 exp 17 p(-1) BI2 V. This is sufficient for rapid particles to give rise to electron-positron pairs in a strong magnetic field, provided that the rotation of the star is not too slow. In this way, electrons and positrons are constantly generated in closed regions of the magnetosphere and accumulate there if they are caught in electrostatic traps located at the ends of magnetic force lines. The electric fields of the traps oscillate and can give rise to both electrons and positrons.
Istomin Ya N.
Mosyagin D. V.
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