General relativistic calculation of magnetic field and Power loss for a misaligned pulsar
arXiv:2111.14439 · doi:10.1016/j.jheap.2022.03.002
Abstract
In this study, we model a pulsar as a general relativistic oblique rotator, where the oblique rotator is a rotationally deformed neutron star whose rotation and magnetic axis are inclined at an angle. The oblique rotator spins down, losing rotational energy through the magnetic poles. The magnetic field is assumed to be dipolar; however, the star has a non-zero azimuthal component due to the misalignment. The magnetic field induces an electric field for a force-free condition. The magnetic field decreases as the misalignment increases and is minimum along the equatorial plane of the star. In contrast, the electric field remains almost constant initially but decreases rapidly at a high misalignment angle. The charge separation at the star surface is qualitatively similar to that of Newtonian calculation. We find that the power loss for a general relativistic rotator is minimum for either an aligned or an orthogonal rotator, which contrasts with Newtonian calculation, where the power loss increases with an increase in the misalignment angle.
19 page, 10 figures
References in corpus (8)
- PSR J0030+0451 Mass and Radius from NICER Data and Implications for the Properties of Neutron Star Matter
- A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation
- Non-rotating and rotating neutron stars in the extended field theoretical model
- Electrodynamics of pulsar magnetospheres
- Strangelet propagation and cosmic ray flux
- Theory of pulsar magnetosphere and wind
- The conversion of Neutron star to Strange star : A two step process
- Radiation from an off-centred rotating dipole in vacuum