Estimates of the Surface Magnetic Field Strength of Radio Pulsars
arXiv:2308.06439 · doi:10.3390/universe9070334
Abstract
We investigate the geometry of the magnetic field of rotation-powered pulsars. A new method for calculating an angle () between the spin and magnetic dipole axes of a neutron star (NS) in the ejector stage is considered within the frame of the magnetic dipole energy loss mechanism. We estimate the surface magnetic field strength () for a population of known neutron stars in the radio pulsar (ejector) stage. The evaluated may differ by an order of magnitude from the values without considering the angle . It is shown that lies in the range -- for a known population of short and middle periodic radio pulsars.
arXiv comment12 pages, 6 figures, 5 tables, 29 references. Published in Universe in the Special Issue Remo Ruffini Festschrift
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