Suzaku Observation of GRS 1915+105: Evolution of Accretion Disc Structure during Limit-Cycle Oscillation

TL;DR

This study analyzes Suzaku X-ray data of GRS 1915+105, revealing how the accretion disk and corona evolve during limit-cycle oscillations, with implications for disk wind, reflection, and corona geometry.

Contribution

It provides detailed spectral analysis showing the evolution of accretion disk structure and corona properties during different states of GRS 1915+105, including the role of non-thermal electrons.

Findings

Strong Comptonization dominates spectra in both states.

Disk wind is detected with ionization correlating with flux.

Reflection varies, indicating changes in corona geometry.

Abstract

We present results from the Suzaku observation of the microquasar GRS 1915+105 performed during the 2005 October multiwavelength campaign. The data include both stable state (class \chi) and limit-cycle oscillation (class \theta). Correct interstellar absorption as well as effects of dust scattering are fully taken into account in the spectral analysis. The energy spectra in the 2-120 keV band in both states are all dominated by strong Comptonization of disk photons by an optically thick (\tau ~7-10) and low temperature (T_e ~2-3 keV) hybrid plasmas containing non-thermal electrons produced with 10-60% of the total power input. Absorption lines of highly ionized Fe ions detected during the oscillation indicate that a strong disk wind is developed. The ionization stage of the wind correlates with the X-ray flux, supporting the photoionization origin. The iron-K emission line shows a strong variability during the oscillation; the reflection is strongest during the dip but disappears during the flare. We interpret this as evidence for "self-shielding" that the Comptonizing corona becomes geometrically thick in the flare phase, preventing photons from irradiating the outer disk. The low-temperature and high luminosity disk emission suggests that the disk structure is similar to that in the very high state of canonical black hole binaries. The spectral variability during the oscillation is explained by the change of the disk geometry and of the physical parameters of Comptonizing corona, particularly the fractional power supplied to the acceleration of non-thermal particles.