V. M. Kontorovich, A. B. Flanchik
Pulsars are the fast rotating neutron stars with strong magnetic field
emitting over a wide frequency range. In spite of the efforts during 40 years
after the discovery of pulsars, the mechanism of their radio emission remains
to be unknown so far. We propose a new approach to solving this problem. The
object of our study is a sample of pulsars with a high-frequency break of the
spectrum from Pushchino catalogue. A theoretical explanation of the observed
dependence of the high-frequency break from the pulsar period is given. The
dependence of the break position from the magnetic field is predicted. This
explanation is based on a new mechanism for electron emission in the inner
polar gap. Radiation occurs when electrons are accelerated in the electric
field rising from zero at the star surface. Acceleration passes through a
maximum and tends to zero when the electron velocity approaches the velocity of
light. The all radiated power is allocated to the radio band. The averaging
over the polar cap, with some natural assumptions of the coherence of the
radiation, leads to the observed spectra, as well as to an acceptable estimate
of the power of radio emission. The same process responsible for the
high-frequency break explains the disappearance of the main pulse of the Crab
pulsar in this frequency range, as well as increasing of the interpulse
amplitude.
View original:
http://arxiv.org/abs/1201.0261
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