Estimates of the Surface Magnetic Field Strength of Radio Pulsars
Kim V. Umirbayeva A. Aimuratov Y.
July 2023Multidisciplinary Digital Publishing Institute (MDPI)
Universe
2023#9Issue 7
We investigate the geometry of the magnetic field of rotation-powered pulsars. A new method for calculating an angle ((Formula presented.)) 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 ((Formula presented.)) for a population of known neutron stars in the radio pulsar (ejector) stage. The evaluated (Formula presented.) may differ by an order of magnitude from the values without considering the angle (Formula presented.). It is shown that (Formula presented.) lies in the range (Formula presented.) – (Formula presented.) for a known population of short and middle periodic radio pulsars.
magnetic dipole radiation , magnetic field , neutron star , radio pulsar
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Fesenkov Astrophysical Institute, Observatory 23, Almaty, 050020, Kazakhstan
Pulkovo Observatory, Pulkovoskoe Shosse 65/1, Saint Petersburg, 196140, Russian Federation
Department of Theoretical and Nuclear Physics, Faculty of Physics and Technology, Al-Farabi Kazakh National University, Al-Farabi Avenue 71, Almaty, 050040, Kazakhstan
International Center for Relativistic Astrophysics Network, Piazza della Repubblica 10, Pescara, 65122, Italy
Fesenkov Astrophysical Institute
Pulkovo Observatory
Department of Theoretical and Nuclear Physics
International Center for Relativistic Astrophysics Network
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