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 ($B_{ \rm ns}$) for a population of known neutron stars in the radio pulsar (ejector) stage. The evaluated $B_{ \rm ns}(\beta)$ may differ by an order of magnitude from the values without considering the angle $\beta$. It is shown that $B_{ \rm ns}(\beta)$ lies in the range $10^{ 8}$--$10^{ 14}\,\text{ G}$ for a known population of short and middle periodic radio pulsars.
Categories: astro-ph.HE