  Ultra-fast outflows (UFOs) have been detected in the high-quality X-ray
spectra of a number of active galactic nuclei (AGN) with fairly high accretion
rates and are thought to significantly contribute to the AGN feedback. After a
decade of dedicated study, their launching mechanisms and structure are still
not well understood, but variability techniques may provide useful constraints.
In this work, therefore, we perform a flux-resolved X-ray spectroscopy on a
highly accreting and variable NLS1 AGN, 1H 0707-495, using all archival
XMM-Newton observations to study the structure of the UFO. We find that the
wind spectral lines weaken at higher luminosities, most likely due to an
increasing ionization parameter as previously found in a few similar sources.
Instead, the velocity is anticorrelated with the luminosity, which is opposite
to the trend observed in the NLS1 IRAS 13224-3809. Furthermore, the detection
of the emission lines, which are not observed in IRAS 13224-3809, indicates a
wind with a larger opening angle in 1H 0707-495, presumably due to a higher
accretion rate. The emitting gas is found to remain broadly constant with the
luminosity. We describe the variability of the wind with a scenario where the
strong radiation extends the launch radius outwards and shields the outer
emitting gas, similarly to super-Eddington compact objects, although other
possible explanations are discussed. Our work provides several hints for a
multi-phase outflow in 1H 0707-495.
