• Publications
  • Influence
Diamagnetic screening of the magnetic field in accreting neutron stars
A possible mechanism for screening of the surface magnetic field of an accreting neutron star, by the accreted material, is investigated. We model the material flow in the surface layers of the star
Magnetic field evolution of accreting neutron stars ⋆ III
We investigate the evolution of the magnetic field of isolated pulsars and of neutron stars in different kinds of binary systems, assuming the field to be originally confined to the crust. Our
Magnetic Fields of Neutron Stars
This article briefly reviews our current understanding of the evolution of magnetic fields in neutron stars, which basically defines the evolutionary pathways between different observational classes
The magnetic fields of millisecond pulsars in globular clusters
Many of the characteristic properties of the millisecond pulsars found in globular clusters are markedly different from those in the Galactic disc. We find that one such physical parameter is the
Evolution of the multipolar magnetic field in isolated neutron stars
The evolution of the multipolar structure of the magnetic field of isolated neutron stars is studied assuming the currents to be confined to the crust. We find that, except for multipoles of very
Gravitational excitation of high frequency QPOs (Research Note)
We discuss the possibility that high-frequency QPOs in neutron-star binary systems may result from forced resonant oscillations of matter in the innermost parts of the accretion disc, excited by
Glitch Statistics of Radio Pulsars : Multiple populations
There appears to be more than one statistically different populations in the energy distribution of glitches, strongly indicative of different mechanisms accessing different energy ranges responsible
The micro-glitch in PSR B1821−24: a case for a strange pulsar?
The single glitch observed in PSR B1821-24, a millisecond pulsar in M28, is unusual on two counts. First, the magnitude of this glitch is at least an order of magnitude smaller (Δν/ν∼10 -11 ) than
Torque decay in the pulsar $(P,\dot{P})$ diagram - Effects of crustal ohmic dissipation and alignment
We investigate the evolution of pulsars in the $(P,\dot{P})$ diagram. We first present analytical formulae to follow the evolution of a pulsar using simple exponential models for magnetic field decay