Rotational and X-ray luminosity evolution of high-B radio pulsars

Benli O., Ertan Ü.

New Astronomy, vol.61, pp.78-83, 2018 (SCI-Expanded) identifier identifier

  • Publication Type: Article / Article
  • Volume: 61
  • Publication Date: 2018
  • Doi Number: 10.1016/j.newast.2017.12.005
  • Journal Name: New Astronomy
  • Journal Indexes: Science Citation Index Expanded (SCI-EXPANDED), Scopus
  • Page Numbers: pp.78-83
  • Keywords: Accretion, Accretion discs, Magnetic fields, Stars: Pulsars: Individual (HBRPs), X-rays: Stars
  • TED University Affiliated: No


In continuation of our earlier work on the long-term evolution of the so-called high–B radio pulsars (HBRPs) with measured braking indices, we have investigated the long-term evolution of the remaining five HBRPs for which braking indices have not been measured yet. This completes our source-by-source analyses of HBRPs in the fallback disc model that was also applied earlier to anomalous X-ray pulsars (AXPs), soft gamma repeaters (SGRs), and dim isolated neutron stars (XDINs). Our results show that the X-ray luminosities and the rotational properties of these rather different neutron star populations can be acquired by neutron stars with fallback discs as a result of differences in their initial conditions, namely the initial disc mass, initial period and the dipole field strength. For the five HBRPs, unlike for AXPs, SGRs and XDINs, our results do not constrain the dipole field strengths of the sources. We obtain evolutionary paths leading to the properties of HBRPs in the propeller phase with dipole fields sufficiently strong to produce pulsed radio emission.