http://arxiv.org/abs/2304.03702
The recent discovery of a radio-emitting neutron star with an ultralong spin period of 76 s, PSR J0901-4046, raises a fundamental question on how such a slowly rotating magnetized object can be active in the radio band. A canonical magnetic field of $1.3\times10^{14}$ G estimated from the pulsar period and its time derivative is wholly insufficient for PSR J0901-4046 to operate. Consideration of a magnetic inclination angle of $10^\circ$ estimated from the pulse width gives a higher magnetic field of $1.5\times10^{15}$ G, which is still an order of magnitude lower than the necessary minimum of $2.5\times10^{16}$ G following from the death line for radio pulsars with magnetic fields exceeding the critical value $4.4\times10^{13}$ G. We show that if the observed microstructure of single pulses reflects relativistic beaming, the inferred surface magnetic field appears to be $3.2\times10^{16}$ G, and without this assumption it is no less than $2.7\times10^{16}$ G, which explains the existence of radio emission from PSR J0901-4046. This estimation makes PSR J0901-4046 a radio pulsar with the strongest magnetic field known and is a sign that PSR J0901-4046 slows down not by magnetic-dipole radiation, but rather by an electric current of 56 MA, when rotational energy is expended in accelerating charged particles over the polar cap.
D. Sob’yanin
Mon, 10 Apr 23
12/36
Comments: 6 pages
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