Observing Rayleigh–Taylor Stable and Unstable Accretion Through a Kalman Filter Analysis of X-Ray Pulsars in the Small Magellanic Cloud

Abstract

Global, three-dimensional magnetohydrodynamic simulations of Rayleigh–Taylor instabilities at the disk–magnetosphere boundary of rotating, magnetized compact stellar objects reveal that accretion occurs in three regimes: the stable regime, the chaotic unstable regime, and the ordered unstable regime. Here we track stochastic fluctuations in the pulse period P ( t ) and aperiodic X-ray luminosity L ( t ) time series of 24 accretion-powered pulsars in the Small Magellanic Cloud using an unscented Kalman filter to analyze Rossi X-ray Timing Explorer data. We measure time-resolved histories of the magnetocentrifugal fastness parameter ω ( t ) and we connect ω ( t ) with the three Rayleigh–Taylor accretion regimes. The 24 objects separate into two distinct groups, with 10 accreting in the stable regime and 14 accreting in the ordered unstable regime. None of the 24 objects except SXP 293 visit the chaotic unstable regime for sustained intervals, although several objects visit it sporadically. The Kalman filter output also reveals a positive temporal cross-correlation between ω ( t ) and the independently measured pulse amplitude A ( t ), which agrees with simulation predictions regarding the pulse-forming behavior of magnetospheric funnel flows in the three accretion regimes.

Keywords

• High mass x-ray binary stars
• Small Magellanic Cloud
• High energy astrophysics
• Binary pulsars