On the magnetic field evolution in isolated neutron stars
We examine the discrepancy between the theoretically expected number of detectable isolated old neutron stars (102-103), and the actually detected number of candidates (2-3). We argue that this discrepancy is explicable in terms of the suppression of accretion from the interstellar medium onto the old neutron stars. We show that for such a suppression to occur, a specific pattern for the magnetic field evolution in neutron stars is required. Strong magnetic fields (B ≳ 1012 G) are required to decay rapidly, while fields of the order of 1010 G are required to remain constant in the absence of accretion. The required pattern agrees with recent theoretical models for magnetic field decay in neutron stars. © 1998. The American Astronomical Society. All rights reserved.
Publication Source (Journal or Book title)
Livio, M., Chun, X., & Frank, J. (1998). On the magnetic field evolution in isolated neutron stars. Astrophysical Journal, 492 (1 PART I), 298-300. https://doi.org/10.1086/305034