Estimates of the Surface Magnetic Field Strength of Radio Pulsars

Abstract

We investigate the geometry of the magnetic field of rotation-powered pulsars. A new method for calculating an angle ($\beta$) 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 ($B_{\mathrm{ns}}$) for a population of known neutron stars in the radio pulsar (ejector) stage. The evaluated $B_{\mathrm{ns}}(\beta )$ may differ by an order of magnitude from the values without considering the angle $\beta$. It is shown that $B_{\mathrm{ns}}(\beta )$ lies in the range $10^8$--$10^{14}\text{G}$ for a known population of short and middle periodic radio pulsars.

12 pages, 6 figures, 5 tables, 29 references. Published in Universe in the Special Issue Remo Ruffini Festschrift

References in corpus (4)

• The physics of strong magnetic fields in neutron stars
• Magnetic angle evolution in accreting neutron stars
• Pulsar radio emission mechanism II. On the origin of relativistic Langmuir solitons in pulsar plasma
• On the evolution of high-B radio pulsars with measured braking indices

Cited by in corpus (1)

• Nethotrons: exploring the possibility of measuring relativistic spin precessions, from Earth's satellites to the Galactic Centre