2003/09/15 by Hongsu Kim, Hyung Mok Lee, Kim, Hongsu +5
Earth and Planetary Sciences · Engineering · Physics and Astronomy · #Astrophysics (astro-ph) #FOS: Physical sciences #General Relativity and Quantum Cosmology (gr-qc) #Geophysics and Gravity Measurements #Geophysics and Sensor Technology #Pulsars and Gravitational Waves Research #astro-ph #gr-qc
paper · pdf · doi:10.48550/arxiv.astro-ph/0309389
22 pages, Revtex4, References added
openalex publication_date 2003/09/15 · arxiv created 2003/09/18 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
In association with the Goldreich-Julian's magnetic braking mechanism to explain the luminosity of radio pulsars as a result of their spin-down, it is of some interest to explore how much of magnetic flux can actually penetrate the surface of the rotating neutron stars at least in idealized situations. In order to address this issue, one needs to figure out the amount of charge on and the structure of magnetic field around a rotating neutron star. In the present work, based on the solution-generating method given by Wald, the magnetic fields around both the uncharged and (slightly) charged neutron star have been obtained. Particularly for the charged neutron star, it has been demonstrated following again the argument by Wald that the neutron star will gradually accrete the charge until it reaches the equilibrium value Q=2B0J. Then next, the magnetic flux through one half of the surface of the rotating neutron star has been computed as well. With the nonvanishing accretion charge having value in the range 0 < Q ≤ 2B0J, the total magnetic flux through the neutron star has been shown to be greater than that without the accretion charge.