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We report on CO and HI studies of the mixed-morphology supernova remnant(SNR) G346.6$-$0.2. We find a wind-blown bubble along the radio continuum shellwith an expansion velocity of $\sim10$ km s$^{-1}$, which was likely formed bystrong stellar winds from the high-mass progenitor of the SNR. The radialvelocities of the CO/HI bubbles at $V_\mathrm{LSR} = -82$-$-59$ km s$^{-1}$ arealso consistent with those of shock-excited 1720 MHz OH masers. The molecularcloud in the northeastern shell shows a high-kinetic temperature of $\sim60$ K,suggesting that shock-heating occurred. The HI absorption studies imply thatG346.6$-$0.2 is located on the far side of the Galactic center from us, and thekinematic distance of the SNR is derived to be $11.1_{-0.3}^{+0.5}$ kpc. Wefind that the CO line intensity has no specific correlation with the electrontemperature of recombining plasma, implying that the recombining plasma inG346.6$-$0.2 was likely produced by adiabatic cooling. With our estimates ofthe interstellar proton density 280 cm$^{-3}$ and gamma-ray luminosity $< 5.8\times 10^{34}$ erg s$^{-1}$, the total energy of accelerated cosmic rays$W_{\rm p} < 9.3 \times 10^{47}$ erg is obtained. A comparison of theage-$W_{\rm p}$ relation to other SNRs suggests that most of the acceleratedcosmic rays in G346.6$-$0.2 have been escaped from the SNR shell.

Discovery of a Wind-Blown Bubble Associated with the Supernova Remnant G346.6-0.2: A Hint for the Origin of Recombining Plasma