Theoretical Analysis of the RX J0209.6-7427 X-ray Spectrum During Giant Outburst

TL;DR

This paper presents a physics-based theoretical model that successfully reproduces the X-ray spectra of RX J0209.6-7427 during a super-Eddington outburst, providing insights into accretion physics across different luminosity states.

Contribution

It is the first to model both low and high luminosity states of an accretion-powered X-ray pulsar using a comprehensive physics-based approach.

Findings

Outer polar cap radius remains constant with luminosity

Column becomes more filled at higher luminosity

Comptonized bremsstrahlung dominates spectral formation

Abstract

We model the spectral formation occurring in the binary X-ray pulsar RX~J0209.6-7427 during the 2019 super-Eddington outburst. Using a theoretical model previously developed by the authors, we are able to produce spectra that closely resemble the phase-averaged X-ray spectra observed using NuSTAR and Insight-HXMT during low and high luminosity states of the outburst, respectively. The theoretical model simulates the accretion of fully ionized gas in a dipole magnetic field, and includes a complete description of the radiation hydrodynamics, matter distribution, and spectral formation. Type II X-ray outbursts provide an opportunity to study accretion over a large range of luminosities for the same neutron star. The analysis performed here represents the first time both the outburst low and high states of an accretion-powered X-ray pulsar are modeled using a physics-based model rather than standard phenomenological fitting with arbitrary mathematical functions. We find the outer polar cap radius remains constant and the column is more fully-filled with increasing luminosity, Comptonized bremsstrahlung dominates the formation of the phase-averaged X-ray spectrum, and a negative correlation exists between cyclotron centroid energy and luminosity, as expected. The super-Eddington nature of the outburst is rendered possible due to the low scattering cross section for photons propagating parallel to the magnetic field. We also find emission through the column top dominates in both the low and high states, implying the pulse profiles should have a roughly sinusoidal shape, which agrees with observed properties of ultra-luminous X-ray pulsars.