Rotational Evolution of The Slowest Radio Pulsar PSR J0250+5854. (arXiv:1901.00300v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Kou_F/0/1/0/all/0/1">F.F. Kou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tong_H/0/1/0/all/0/1">H.Tong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Xu_R/0/1/0/all/0/1">R. X. Xu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhou_X/0/1/0/all/0/1">X. Zhou</a>
We apply theoretical spin-down models of magentospheric evolution and
magentic field decay to simulate the possible evolution of PSR J0250+5854,
which is the slowest-spinning radio pulsar by now. It is possible that PSR
J0250+5854 has a small inclination angle but a relatively high magnetic field
by considering the alignment of inclination angle in a 3-D magnetosphere. Our
calculations show that PSR J0250+5854 may be an old high magnetic field pulsar
or magnetar. In this case, the clustering of similarly long-period pulsars
would have a relatively low period derivative. However, by considering the
magnetic field decay, calculations show possible connection between PSR
J0250+5854 and high dipole-magnetic field magentars. In this case, similarly
long-period pulsars will have a relatively high period derivative. Future
observations of more long period pulsars will help to distinguish these two
cases.
We apply theoretical spin-down models of magentospheric evolution and
magentic field decay to simulate the possible evolution of PSR J0250+5854,
which is the slowest-spinning radio pulsar by now. It is possible that PSR
J0250+5854 has a small inclination angle but a relatively high magnetic field
by considering the alignment of inclination angle in a 3-D magnetosphere. Our
calculations show that PSR J0250+5854 may be an old high magnetic field pulsar
or magnetar. In this case, the clustering of similarly long-period pulsars
would have a relatively low period derivative. However, by considering the
magnetic field decay, calculations show possible connection between PSR
J0250+5854 and high dipole-magnetic field magentars. In this case, similarly
long-period pulsars will have a relatively high period derivative. Future
observations of more long period pulsars will help to distinguish these two
cases.
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