Unifying neutron star sub-populations in the supernova fallback accretion model

TL;DR

This paper uses a supernova fallback disk model to simulate the spin and magnetic field evolution of young neutron stars, unifying various sub-populations like magnetars, CCOs, and pulsars under one framework.

Contribution

It demonstrates that the supernova fallback accretion model can explain the diversity of young neutron star sub-populations and their observed properties.

Findings

The model accounts for weak magnetic fields of CCOs.

It reproduces measured braking indices of young pulsars.

Evolutionary links among NS sub-populations are established.

Abstract

We employ the supernova fallback disk model to simulate the spin evolution of isolated young neutron stars (NSs). We consider the submergence of the NS magnetic fields during the supercritical accretion stage and its succeeding reemergence. It is shown that the evolution of the spin periods and the magnetic fields in this model is able to account for the relatively weak magnetic fields of central compact objects and the measured braking indices of young pulsars. For a range of initial parameters, evolutionary links can be established among various kinds of NS sub-populations including magnetars, central compact objects and young pulsars. Thus, the diversity of young NSs could be unified in the framework of the supernova fallback accretion model.