Using laboratory time-resolved emission spectra to benchmark models for accretion-powered objects

Accretion-powered objects are among the most luminous objects in the universe. Spectral observations of these systems have revealed time-dependent behavior, demonstrated in the form of warm absorber outflows in AGN and type I X-ray bursts in low mass X-ray binaries. The recent implementation of time-dependence in astrophysical photoionized plasma models necessitates scrutiny of the underlying atomic kinetics.



The Z-facility at Sandia National Labs has a unique capability to probe the relevant physics. On the accretion-powered objects platform, X-rays from the rapidly evolving Z-pinch irradiate a foil target which reaches temperature, density, and photoionization conditions found in accretion disks. This provides a means to benchmark photoionized plasma codes (such as XSTAR) by measuring reproducible, high resolution, time-resolved emission spectra.



We present state-of-the-art time-resolved emission data collected on the platform. We show preliminary data-model comparisons for emission intensity and results of simulations performed with the 1-D radiation hydrodynamics code HELIOS-CR. These simulations address questions of plasma gradients, charge state distribution evolution, and expansion dynamics. Results from these simulations will elucidate the spectroscopic analysis of the data and facilitate more effective data-model comparisons.