Looking into the Theory of Pulsar Accretion: Cen X-3 and XTE J1946+274

TL;DR

This paper reviews pulsar accretion physics and introduces a new spectral modeling tool applied to Suzaku data of two pulsars, providing a step towards a physical understanding of their X-ray spectra.

Contribution

It presents a new implementation of a physical continuum model for pulsar accretion, applied to real data of Cen X-3 and XTE J1946+274, advancing spectral analysis methods.

Findings

Model successfully fits spectra of Cen X-3 and XTE J1946+274

First physical spectral descriptions of these pulsars

Demonstrates potential for constraining accretion physics

Abstract

This is an overview of pulsar accretion modeling. The physics of pulsar accretion, i.e., the process of plasma flow onto the neutron star surface, can be constrained from the spectral properties of the X-ray source. We discuss a new implementation of the physical continuum model developed by Becker and Wolff (2007, ApJ 654, 435). The model incorporates Comptonized blackbody, bremsstrahlung, and cyclotron emission. We discuss preliminary results of applying the new tool to the test cases of Suzaku data of Cen X-3 and XTE J1946+274. Cen X-3 is a persistent accreting pulsar with an O-star companion observed during a bright period. XTE J1946+274 is a transient accreting pulsar with a Be companion observed during a dim period. Both sources show spectra that are well described with an empirical Fermi Dirac cutoff power law model. We extend the spectral analysis by making the first steps towards a physical description of Cen X-3 and XTE J1946+274.