Super-Eddington Emission from Accreting, Highly Magnetised Neutron Stars with a Multipolar Magnetic Field

TL;DR

This paper models how highly magnetized neutron stars with complex magnetic fields can produce super-Eddington luminosities observed in pulsating ultra-luminous X-ray sources, challenging previous assumptions of purely dipolar fields.

Contribution

It extends existing models by incorporating multipolar magnetic field topologies to explain super-Eddington emissions from accreting neutron stars.

Findings

Maximum luminosity depends on magnetic field strength near the NS surface.

A neutron star with specific multipolar magnetic field components can reach luminosities of ~10^{41} erg/s.

The model explains observed properties of two specific PULXs, NGC 5907 ULX-1 and NGC 7793 P13.

Abstract

Pulsating ultra-luminous X-ray sources (PULXs) are characterised by an extremely large luminosity ($ > 10^{40} \text{erg s}^{-1}$). While there is a general consensus that they host an accreting, magnetized neutron star (NS), the problem of how to produce luminosities $> 100$ times the Eddington limit, $L_E$, of a solar mass object is still debated. A promising explanation relies on the reduction of the opacities in the presence of a strong magnetic field, which allows for the local flux to be much larger than the Eddington flux. However, avoiding the onset of the propeller effect may be a serious problem. Here, we reconsider the problem of column accretion onto a highly magnetized NS, extending previously published calculations by relaxing the assumption of a pure dipolar field and allowing for more complex magnetic field topologies. We find that the maximum luminosity is determined primarily by the magnetic field strength near the NS surface. We also investigate other factors determining the accretion column geometry and the emergent luminosity, such as the assumptions on the parameters governing the accretion flow at the disk-magnetosphere boundary. We conclude that a strongly magnetized NS with a dipole component of $\sim 10^{13} \text{G}$, octupole component of $\sim10^{14} \text{G}$ and spin period $\sim1 \text{s}$ can produce a luminosity of $\sim 10^{41} \text{erg s}^{-1}$ while avoiding the propeller regime. We apply our model to two PULXs, NGC 5907 ULX-1 and NGC 7793 P13, and discuss how their luminosity and spin period rate can be explained in terms of different configurations, either with or without multipolar magnetic components.