Pulsar Magnetic Field Oscillation Model and Verification Methods

TL;DR

The paper introduces the MO model, a magnetic field oscillation framework for pulsars, explaining various phenomena and verified through eight methods, also applicable to other magnetic stars.

Contribution

It presents a novel magnetic field oscillation model for pulsars, offering comprehensive explanations and verification methods, extending to non-compact magnetic stars.

Findings

Explains pulsar polarization, glitches, and precession.

Provides verification methods for the MO model.

Applicable to ultracool dwarfs and chemically peculiar stars.

Abstract

We constructed the magnetic field oscillation model (hereafter the MO model) by analogizing the periodically reversing phenomenon of the solar magnetic field to pulsars. Almost all kinds of pulsar radiation phenomena are best explained using the MO model, especially polarization characteristics, glitch, generation rate, the geodetic precession of pulsars and the configuration of pulsar-wind nebula of the Crab. The MO model also provides satisfactory explanation for other characteristics of pulsars, e.g., interpulse, spin-down, pulse nulling, beat and pulse drift, the loss rate of the rotating energy, and the accuracy of frequency. We present eight verification methods for the MO model. In addition to pulsars, our MO model can also be used to explain the pulse emission from non-compact stars such as the ultracool dwarf TVLM 513-46546 and the magnetic chemically peculiar star CU Virginis.