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Particle acceleration physics at supernova remnant (SNR) shocks is one of themost intriguing problems in astrophysics. SNR RCW~86 provides a suitableenvironment for understanding the particle acceleration physics because one canextract the information of both accelerated particles and accelerationenvironment at the same regions through the bright X-ray emission. In thiswork, we study X-ray proper motions and spectral properties of the southwesternregion of RCW~86. The proper motion velocities are found to be $\sim300$--2000~km~s$^{-1}$ at a distance of 2.8~kpc. We find two inward-movingfilaments, which are more likely reflected shocks rather than reverse shocks.Based on the X-ray spectroscopy, we evaluate thermal parameters such as theambient density and temperature, and non-thermal parameters such as thepower-law flux and index. From the flux decrease in time of several non-thermalfilaments, we estimate the magnetic field amplitudes to be $\sim30$--100~$\mu$G. Gathering the physical parameters, we then investigateparameter correlations. We find that the synchrotron emission fromthermal-dominated filaments is correlated with the ambient density $n_{\rm e}$as $\text{(power-law flux)} \propto n_{\rm e}^{1.0 \pm 0.2}$ and$\text{(power-law index)} \propto n_{\rm e}^{0.38 \pm 0.10}$, not or onlyweakly with the shock velocity and shock obliquity. As an interpretation, wepropose a shock-cloud interaction scenario, where locally enhanced magneticturbulence levels have a great influence on local acceleration conditions.

Particle acceleration controlled by ambient density in the southwestern rim of RCW 86