8 research outputs found
On The Recently Discovered Pulsations From RX J1856.5-3754
An explanation of the recently discovered 7 s pulsations from the isolated
neutron star RX J1856.5-3754 is presented. It is assumed that the real spin
period of this source is s, whereas the observed spin-modulation is
caused by the presence of a nearly transverse, very low frequency drift waves
in the pulsar magnetosphere. It is supposed that the period of the drift wave
is equal to a recently observed one. The simulated lightcurve is plotted, the
angular parameters are defined and the value of the pulsed fraction of only
is explained.Comment: 7 pages, 2 figure
PSR J0737-3039B: A probe of radio pulsar emission heights
In the double pulsar system PSR J0737-3039A/B the strong wind produced by
pulsar A distorts the magnetosphere of pulsar B. The influence of these
distortions on the orbital-dependent emission properties of pulsar B can be
used to determine the location of the coherent radio emission generation region
in the pulsar magnetosphere. Using a model of the wind-distorted magnetosphere
of pulsar B and the well defined geometrical parameters of the system, we
determine the minimum emission height to be ~ 20 neutron star radii in the two
bright orbital longitude regions. We can determine the maximum emission height
by accounting for the amount of deflection of the polar field line with respect
to the magnetic axis using the analytical magnetic reconnection model of Dungey
and the semi-empirical numerical model of Tsyganenko. Both of these models
estimate the maximum emission height to be ~ 2500 neutron star radii. The
minimum and maximum emission heights we calculate are consistent with those
estimated for normal isolated pulsars.Comment: 29 pages, 14 figures, Accepted by ApJ on 3 March 201
On the nature of radio pulsars with long periods
It is shown that the drift waves near the light cylinder can cause the
modulation of the emission with periods of the order several seconds. These
periods explain the intervals between successive pulses observed in "magnetars"
and radio pulsars with long periods. The model under consideration makes it
possible to calculate the real rotation periods of the host neutron stars. They
are less than 1 sec for the investigated objects. The magnetic fields at the
surface of the neutron star of the order 10^(11)-10^(13) G and equal to the
usual fields for known radio pulsarsComment: 18 pages, 4 figure