Constraints on the internal physics of neutron stars from the observational data of several young pulsars: the role of a power-law decaying dipole magnetic field

Abstract

The observational data (e.g., the timing data and magnetic tilt angles $\chi$) of young pulsars can be used to probe some critical issues about the internal physics of neutron stars (NSs), for instance, the number of precession cycles $\xi$ and the internal magnetic field configuration (IMFC) of NSs. Evolution of the dipole magnetic field $B_{\mathrm{d}}$ of NSs may play an important role in determining the final results. In this work, a power-law form is adopted to describe the decay of $B_{\mathrm{d}}$. In such a scenario, the IMFC and $\xi$ of young pulsars with an ordinary $B_{\rm d}\sim10^{12}-\-10^{13}$ G and a steady braking index $n$ are investigated. Since the tilt angle change rates $\dot{\chi }$ of pulsars with $n<3$ can be theoretically predicted, a test on the power-law decay model can thus be made by comparing the theoretical values to that obtained from observations. However, such a comparison can only be made on the Crab pulsar currently, and the results show that the power-law decay model is inconsistent with the Crab's observations. We suggest that rather than decay, the Crab's $B_{\mathrm{d}}$ should increase with time at a rate $\sim 12-14$ G/s. A definite conclusion on the validity of the power-law decay model for pulsars with ordinary $B_{\mathrm{d}}$ may be given if $\dot{\chi }$ of other pulsars could be measured.

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Cited by in corpus (2)

• Dense Matter in Neutron Stars with eXTP
• Investigating the neutron star physics through observations of several young pulsars in the dipole-field re-emergence scenario