Complex emission patterns: fluctuations and bistability of polar-cap potentials. (arXiv:2001.09680v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Jones_P/0/1/0/all/0/1">P B Jones</a>
Development of the ion-proton pulsar model extends it to the limit of large
unscreened polar-cap potentials, for example, as in the Vela pulsar, in which
ion charges differ only by small increments from their complete screening
values. It is shown that the atomic number Z of an ion following its passage
from the canonical Z_0 = 26 value through the electromagnetic shower region to
the surface is not necessarily time-independent but can vary between fixed
limits in an irregular or quasi-periodic way in a characteristic time of the
order of 10^4 s. Thus at a certain Z the system may transition to an unstable
state of higher electric potential and it is argued that this is the physical
basis for mode-changes, long-term nulls, periodic or otherwise. The model
requires an orientation of magnetic dipole moment relative to rotational spin
giving a positive corotational charge density. Success of the model would fix
the particle composition of the remaining parts of the magnetosphere, including
the Y-point and is therefore relevant to X-ray and gamma-ray emission
processes.
Development of the ion-proton pulsar model extends it to the limit of large
unscreened polar-cap potentials, for example, as in the Vela pulsar, in which
ion charges differ only by small increments from their complete screening
values. It is shown that the atomic number Z of an ion following its passage
from the canonical Z_0 = 26 value through the electromagnetic shower region to
the surface is not necessarily time-independent but can vary between fixed
limits in an irregular or quasi-periodic way in a characteristic time of the
order of 10^4 s. Thus at a certain Z the system may transition to an unstable
state of higher electric potential and it is argued that this is the physical
basis for mode-changes, long-term nulls, periodic or otherwise. The model
requires an orientation of magnetic dipole moment relative to rotational spin
giving a positive corotational charge density. Success of the model would fix
the particle composition of the remaining parts of the magnetosphere, including
the Y-point and is therefore relevant to X-ray and gamma-ray emission
processes.
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