Properties
of the Emission of Short-Period Pulsars
I. F. Malov
Astrospace
Center, Lebedev Institute of Physics, Russian Academy of
Sciences,
ul. Profsoyuznaya 84/52, Moscow, 117810 Russia
Received November
12, 1996
Abstract—Modern
observational data confirm the hypothesis that short-period
pulsars (P 
0.1 s) are a special group of
objects, with their own emission mechanism and location of the
emission region near the light cylinder. The conventional
assumptions of nonrelativistic rotation (
1) and low plasma energy compared
to the magnetic field energy in the magnetospheres of these
pulsars (specified by the parameter 
) are
incorrect. It is therefore necessary to develop a magnetosphere
model for pulsars with P 
0.1 s for and values
of the order of unity. Plasma instabilities that could be sources
of the observed emission from short-period pulsars are indicated.
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